TY - JOUR A1 - Becker, George D. A1 - Pettini, Max A1 - Rafelski, Marc A1 - Boera, Elisa A1 - Christensen, Lise A1 - Cupani, Guido A1 - Ellison, Sara L. A1 - Farina, Emanuele Paolo A1 - Fumagalli, Michele A1 - Lopez, Sebastian A1 - Neeleman, Marcel A1 - Ryan-Weber, Emma A1 - Worseck, Gabor T1 - The Evolution of OI over 3.2 < z < 6.5: Reionization of the Circumgalactic Medium JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - We present a survey for metal absorption systems traced by neutral oxygen over 3.2 < z < 6.5. Our survey uses Keck/ESI and VLT/X-Shooter spectra of 199 QSOs with redshifts up to 6.6. In total, we detect 74 OI absorbers, of which 57 are separated from the background QSO by more than 5000 km s(-1). We use a maximum likelihood approach to fit the distribution of OI lambda 1302 equivalent widths in bins of redshift and from this determine the evolution in number density of absorbers with W-1302 > 0.05 angstrom, of which there are 49 nonproximate systems in our sample. We find that the number density does not monotonically increase with decreasing redshift, as would naively be expected from the buildup of metal-enriched circumgalactic gas with time. The number density over 4.9 < z < 5.7 is a factor of 1.7-4.1 lower (68% confidence) than that over 5.7 < z < 6.5, with a lower value at z < 5.7 favored with 99% confidence. This decrease suggests that the fraction of metals in a low-ionization phase is larger at z similar to 6 than at lower redshifts. Absorption from highly ionized metals traced by CIV is also weaker in higher-redshift OI systems, supporting this picture. The evolution of OI absorbers implies that metal-enriched circumgalactic gas at z similar to 6 is undergoing an ionization transition driven by a strengthening ultraviolet background. This in turn suggests that the reionization of the diffuse intergalactic medium may still be ongoing at or only recently ended by this epoch. Y1 - 2019 U6 - https://doi.org/10.3847/1538-4357/ab3eb5 SN - 0004-637X SN - 1538-4357 VL - 883 IS - 2 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Wilkin, Kyle J. A1 - Parrish, Robert M. A1 - Yang, Jie A1 - Wolf, Thomas J. A. A1 - Nunes, J. Pedro F. A1 - Gühr, Markus A1 - Li, Renkai A1 - Shen, Xiaozhe A1 - Zheng, Qiang A1 - Wang, Xijie A1 - Martinez, Todd J. A1 - Centurion, Martin T1 - Diffractive imaging of dissociation and ground-state dynamics in a complex molecule JF - Physical review : A, Atomic, molecular, and optical physics N2 - We have investigated the structural dynamics in photoexcited 1,2-diiodotetrafluoroethane molecules (C2F4I2) in the gas phase experimentally using ultrafast electron diffraction and theoretically using FOMO-CASCI excited-state dynamics simulations. The molecules are excited by an ultraviolet femtosecond laser pulse to a state characterized by a transition from the iodine 5p perpendicular to orbital to a mixed 5p parallel to sigma hole and CF2 center dot antibonding orbital, which results in the cleavage of one of the carbon-iodine bonds. We have observed, with sub-Angstrom resolution, the motion of the nuclear wave packet of the dissociating iodine atom followed by coherent vibrations in the electronic ground state of the C2F4I radical. The radical reaches a stable classical (nonbridged) structure in less than 200 fs. Y1 - 2019 U6 - https://doi.org/10.1103/PhysRevA.100.023402 SN - 2469-9926 SN - 2469-9934 VL - 100 IS - 2 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Wolf, Thomas J. A. A1 - Parrish, Robert M. A1 - Myhre, Rolf H. A1 - Martinez, Todd J. A1 - Koch, Henrik A1 - Gühr, Markus T1 - Observation of Ultrafast Intersystem Crossing in Thymine by Extreme Ultraviolet Time-Resolved Photoelectron Spectroscopy JF - The journal of physical chemistry : A, Molecules, spectroscopy, kinetics, environment & general theory N2 - We studied the photoinduced ultrafast relaxation dynamics of the nucleobase thymine using gas-phase time-resolved photoelectron spectroscopy. By employing extreme ultraviolet pulses from high harmonic generation for photoionization, we substantially extend our spectral observation window with respect to previous studies. This enables us to follow relaxation of the excited state population all the way to low-lying electronic states including the ground state. In thymine, we observe relaxation from the optically bright (1)pi pi* state of thymine to a dark (1)n pi* state within 80 +/- 30 fs. The (1)n pi* state relaxes further within 3.5 +/- 0.3 ps to a low-lying electronic state. By comparison with quantum chemical simulations, we can unambiguously assign its spectroscopic signature to the (3)pi pi* state. Hence, our study draws a comprehensive picture of the relaxation mechanism of thymine including ultrafast intersystem crossing to the triplet manifold. Y1 - 2019 U6 - https://doi.org/10.1021/acs.jpca.9b05573 SN - 1089-5639 SN - 1520-5215 VL - 123 IS - 32 SP - 6897 EP - 6903 PB - American Chemical Society CY - Washington ER - TY - JOUR A1 - Rinaldi, G. A1 - Formisano, M. A1 - Kappel, David A1 - Capaccioni, F. A1 - Bockelee-Morvan, D. A1 - Cheng, Y-C A1 - Vincent, J-B A1 - Deshapriya, P. A1 - Arnold, G. A1 - Capria, M. T. A1 - Ciarniello, M. A1 - De Sanctis, M. C. A1 - Doose, L. A1 - Erard, S. A1 - Federico, C. A1 - Filacchione, G. A1 - Fink, U. A1 - Leyrat, C. A1 - Longobardo, A. A1 - Magni, G. A1 - Mighorini, A. A1 - Mottola, S. A1 - Naletto, G. A1 - Raponi, A. A1 - Taylor, F. A1 - Tosi, F. A1 - Tozzi, G. P. A1 - Salatti, M. T1 - Analysis of night-side dust activity on comet 67P observed by VIRTIS-M BT - a new method to constrain the thermal inertia on the surface JF - Astronomy and astrophysics : an international weekly journal N2 - On 2015 July 18, near perihelion at a heliocentric distance of 1.28 au, the Visible InfraRed Thermal Imaging Spectrometer (VIRTIS-M) on board the Rosetta spacecraft had the opportunity of observing dust activity in the inner coma with a view of the night side (shadowed side) of comet 67P/Churyumov-Gerasimenko. At the time of the measurements we present here, we observe a dust plume that originates on the far side of the nucleus. We are able to identify the approximate location of its source at the boundary between the Hapi and Anuket regions, and we find that it has been in darkness for some hours before the observation. Assuming that this time span is equal to the conductive time scale, we obtain a thermal inertia in the range 25-36 W K-1 m(-2) s(-1/2). These thermal inertia values can be used to verify with a 3D finite-element method (REM) numerical code whether the surface and subsurface temperatures agree with the values found in the literature. We explored three different configurations: (1) a layer of water ice mixed with dust beneath a dust mantle of 5 mm with thermal inertia of 36 J m(-2) K-1 S-0.5 ; (2) the same structure, but with thermal inertia of 100 J m(-2) K-1 S-0.5; (3) an ice-dust mixture that is directly exposed. Of these three configurations, the first seems to be the most reasonable, both for the low thermal inertia and for the agreement with the surface and subsurface temperatures that have been found for the comet 67P/Churyumov-Gerasimenko. The spectral properties of the plume show that the visible dust color ranged from 16 +/- 4.8%/100 nm to 13 +/- 2.6%/100 nm, indicating that this plume has no detectable color gradient. The morphology of the plume can be classified as a narrow jet that has an estimated total ejected mass of between 6 and 19 tons when we assume size distribution indices between -2.5 and -3. KW - comets: general KW - comets: individual: 67P/Churyumov-Gerasimenko KW - infrared: planetary systems Y1 - 2019 U6 - https://doi.org/10.1051/0004-6361/201834907 SN - 1432-0746 VL - 630 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Tubiana, C. A1 - Rinaldi, G. A1 - Guettler, C. A1 - Snodgrass, C. A1 - Shi, X. A1 - Hu, X. A1 - Marschall, R. A1 - Fulle, M. A1 - Bockeele-Morvan, D. A1 - Naletto, G. A1 - Capaccioni, F. A1 - Sierks, H. A1 - Arnold, G. A1 - Barucci, M. A. A1 - Bertaux, J-L A1 - Bertini, I A1 - Bodewits, D. A1 - Capria, M. T. A1 - Ciarniello, M. A1 - Cremonese, G. A1 - Crovisier, J. A1 - Da Deppo, V A1 - Debei, S. A1 - De Cecco, M. A1 - Deller, J. A1 - De Sanctis, M. C. A1 - Davidsson, B. A1 - Doose, L. A1 - Erard, S. A1 - Filacchione, G. A1 - Fink, U. A1 - Formisano, M. A1 - Fornasier, S. A1 - Gutierrez, P. J. A1 - Ip, W-H A1 - Ivanovski, S. A1 - Kappel, David A1 - Keller, H. U. A1 - Kolokolova, L. A1 - Koschny, D. A1 - Krueger, H. A1 - La Forgia, F. A1 - Lamy, P. L. A1 - Lara, L. M. A1 - Lazzarin, M. A1 - Levasseur-Regourd, A. C. A1 - Lin, Z-Y A1 - Longobardo, A. A1 - Lopez-Moreno, J. J. A1 - Marzari, F. A1 - Migliorini, A. A1 - Mottola, S. A1 - Rodrigo, R. A1 - Taylor, F. A1 - Toth, I A1 - Zakharov, V T1 - Diurnal variation of dust and gas production in comet 67P/Churyumov-Gerasimenko at the inbound equinox as seen by OSIRIS and VIRTIS-M on board Rosetta JF - Astronomy and astrophysics : an international weekly journal N2 - Context. On 27 April 2015, when comet 67P/Churyumov-Gerasimenko was at 1.76 au from the Sun and moving toward perihelion, the OSIRIS and VIRTIS-M instruments on board the Rosetta spacecraft simultaneously observed the evolving dust and gas coma during a complete rotation of the comet. Aims. We aim to characterize the spatial distribution of dust, H2O, and CO2 gas in the inner coma. To do this, we performed a quantitative analysis of the release of dust and gas and compared the observed H2O production rate with the rate we calculated using a thermophysical model. Methods. For this study we selected OSIRIS WAC images at 612 nm (dust) and VIRTIS-M image cubes at 612 nm, 2700 nm (H2O emission band), and 4200 nm (CO2 emission band). We measured the average signal in a circular annulus to study the spatial variation around the comet, and in a sector of the annulus to study temporal variation in the sunward direction with comet rotation, both at a fixed distance of 3.1 km from the comet center. Results. The spatial correlation between dust and water, both coming from the sunlit side of the comet, shows that water is the main driver of dust activity in this time period. The spatial distribution of CO2 is not correlated with water and dust. There is no strong temporal correlation between the dust brightness and water production rate as the comet rotates. The dust brightness shows a peak at 0 degrees subsolar longitude, which is not pronounced in the water production. At the same epoch, there is also a maximum in CO2 production. An excess of measured water production with respect to the value calculated using a simple thermophysical model is observed when the head lobe and regions of the southern hemisphere with strong seasonal variations are illuminated (subsolar longitude 270 degrees-50 degrees). A drastic decrease in dust production when the water production (both measured and from the model) displays a maximum occurs when typical northern consolidated regions are illuminated and the southern hemisphere regions with strong seasonal variations are instead in shadow (subsolar longitude 50 degrees-90 degrees). Possible explanations of these observations are presented and discussed. KW - comets: general KW - comets: individual: 67P/Churyumov-Gerasimenko KW - methods: data analysis Y1 - 2019 U6 - https://doi.org/10.1051/0004-6361/201834869 SN - 1432-0746 VL - 630 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Baran, Andrzej S. A1 - Telting, J. H. A1 - Jeffery, C. Simon A1 - Ostensen, R. H. A1 - Vos, Joris A1 - Reed, M. D. A1 - Vŭcković, Maja T1 - K2 observations of the sdBV plus dM/bd binaries PHL457 and EQPsc JF - Monthly notices of the Royal Astronomical Society N2 - We present an analysis of two pulsating subdwarf B stars PHL 457 and EQ Psc observed during the K2 mission. The K2 light curves of both stars show variation consistent with irradiation of a cooler companion by the hot subdwarf. They also show higher frequency oscillations consistent with pulsation. Using new spectroscopic data, we measured the radial velocity, effective temperature, surface gravity, and helium abundance of both hot subdwarfs as a function of orbital phase. We confirm the previously published spectroscopic orbit of PHL 457, and present the first spectroscopic orbit of EQ Psc. The orbital periods are 0.313 and 0.801 d, respectively. For EQPsc, we find a strong correlation between T-eff and orbital phase, due to contribution of light from the irradiated companion. We calculated amplitude spectra, identified significant pulsation frequencies, and searched for multiplets and asymptotic period spacings. By means of multiplets and period spacing, we identified the degrees of several pulsation modes in each star. The g-mode multiplets indicate subsynchronous core rotation with periods of 4.6 d (PHL 457) and 9.4 d (EQ Psc). We made spectral energy disctribution (SED) fits of PHL 457 and EQ Psc using available broad-band photometry and Gaia data. While the SED of PHL 457 shows no evidence of a cool companion, the SED for EQPsc clearly shows an infrared (IR) access consistent with a secondary with a temperature of about 6800K and a radius of 0.23 R-circle dot. This is the first detection of an IR access in any sdB + dM binary. KW - binaries: general KW - stars: individual (PHL 457, EQ Psc) KW - stars: oscillations (including pulsations) Y1 - 2019 U6 - https://doi.org/10.1093/mnras/stz2209 SN - 0035-8711 SN - 1365-2966 VL - 489 IS - 2 SP - 1556 EP - 1571 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Eliazar, Iddo A1 - Metzler, Ralf A1 - Reuveni, Shlomi T1 - Poisson-process limit laws yield Gumbel max-min and min-max JF - Physical review : E, Statistical, nonlinear and soft matter physics N2 - “A chain is only as strong as its weakest link” says the proverb. But what about a collection of statistically identical chains: How long till all chains fail? The answer to this question is given by the max-min of a matrix whose (i,j)entry is the failure time of link j of chain i: take the minimum of each row, and then the maximum of the rows' minima. The corresponding min-max is obtained by taking the maximum of each column, and then the minimum of the columns' maxima. The min-max applies to the storage of critical data. Indeed, consider multiple backup copies of a set of critical data items, and consider the (i,j) matrix entry to be the time at which item j on copy i is lost; then, the min-max is the time at which the first critical data item is lost. In this paper we address random matrices whose entries are independent and identically distributed random variables. We establish Poisson-process limit laws for the row's minima and for the columns' maxima. Then, we further establish Gumbel limit laws for the max-min and for the min-max. The limit laws hold whenever the entries' distribution has a density, and yield highly applicable approximation tools and design tools for the max-min and min-max of large random matrices. A brief of the results presented herein is given in: Gumbel central limit theorem for max-min and min-max Y1 - 2019 U6 - https://doi.org/10.1103/PhysRevE.100.022129 SN - 2470-0045 SN - 2470-0053 VL - 100 IS - 2 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Eliazar, Iddo A1 - Metzler, Ralf A1 - Reuveni, Shlomi T1 - Gumbel central limit theorem for max-min and min-max JF - Physical review : E, Statistical, nonlinear and soft matter physics N2 - The max-min and min-max of matrices arise prevalently in science and engineering. However, in many real-world situations the computation of the max-min and min-max is challenging as matrices are large and full information about their entries is lacking. Here we take a statistical-physics approach and establish limit laws—akin to the central limit theorem—for the max-min and min-max of large random matrices. The limit laws intertwine random-matrix theory and extreme-value theory, couple the matrix dimensions geometrically, and assert that Gumbel statistics emerge irrespective of the matrix entries' distribution. Due to their generality and universality, as well as their practicality, these results are expected to have a host of applications in the physical sciences and beyond. Y1 - 2019 U6 - https://doi.org/10.1103/PhysRevE.100.020104 SN - 2470-0045 SN - 2470-0053 VL - 100 IS - 2 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Poeschel, Thorsten A1 - Brilliantov, Nikolai V. A1 - Formella, Arno T1 - Impact of high-energy tails on granular gas properties JF - Physical review : E, Statistical, nonlinear and soft matter physics N2 - The velocity distribution function of granular gases in the homogeneous cooling state as well as some heated granular gases decays for large velocities as f proportional to exp(-const x nu). That is, its high-energy tail is overpopulated as compared with the Maxwell distribution. At the present time, there is no theory to describe the influence of the tail on the kinetic characteristics of granular gases. We develop an approach to quantify the overpopulated tail and analyze its impact on granular gas properties, in particular on the cooling coefficient. We observe and explain anomalously slow relaxation of the velocity distribution function to its steady state. Y1 - 2006 U6 - https://doi.org/10.1103/PhysRevE.74.041302 SN - 1539-3755 SN - 1550-2376 VL - 74 IS - 4 PB - The American Physical Society CY - College Park ER - TY - JOUR A1 - Baptista, Murilo da Silva A1 - Grebogi, Celso A1 - Koberle, Roland T1 - Dynamically multilayered visual system of the multifractal fly JF - Physical review letters Y1 - 2006 U6 - https://doi.org/10.1103/PhysRevLett.97.178102 SN - 0031-9007 VL - 97 IS - 17 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Hamann, Wolf-Rainer A1 - Graefener, G. A1 - Liermann, A. T1 - The galactic WN stars - Spectral analyses with line-blanketed model atmospheres versus stellar evolution models with and without rotation JF - Astronomy and astrophysics : an international weekly journal N2 - Context. Very massive stars pass through the Wolf-Rayet (WR) stage before they finally explode. Details of their evolution have not yet been safely established, and their physics are not well understood. Their spectral analysis requires adequate model atmospheres, which have been developed step by step during the past decades and account in their recent version for line blanketing by the millions of lines from iron and iron-group elements. However, only very few WN stars have been re-analyzed by means of line-blanketed models yet. Aims. The quantitative spectral analysis of a large sample of Galactic WN stars with the most advanced generation of model atmospheres should provide an empirical basis for various studies about the origin, evolution, and physics of the Wolf-Rayet stars and their powerful winds. Methods. We analyze a large sample of Galactic WN stars by means of the Potsdam Wolf-Rayet (PoWR) model atmospheres, which account for iron line blanketing and clumping. The results are compared with a synthetic population, generated from the Geneva tracks for massive star evolution. Results. We obtain a homogeneous set of stellar and atmospheric parameters for the GalacticWN stars, partly revising earlier results. Conclusions. Comparing the results of our spectral analyses of the Galactic WN stars with the predictions of the Geneva evolutionary calculations, we conclude that there is rough qualitative agreement. However, the quantitative discrepancies are still severe, and there is no preference for the tracks that account for the effects of rotation. It seems that the evolution of massive stars is still not satisfactorily understood. KW - stars : mass-loss KW - stars : winds, outflows KW - stars : Wolf-Rayet KW - stars : atmospheres KW - stars : early-type KW - stars : evolution Y1 - 2006 U6 - https://doi.org/10.1051/0004-6361:20065052 SN - 0004-6361 VL - 457 IS - 3 SP - 1015 EP - 1031 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Zaikin, Alexey A1 - Kurths, Jürgen T1 - Optimal length transportation hypothesis to model proteasome product size distribution JF - Journal of biological physics : emphasizing physical principles in biological research ; an international journal for the formulation and application of mathematical models in the biological sciences N2 - This paper discusses translocation features of the 20S proteasome in order to explain typical proteasome length distributions. We assume that the protein transport depends significantly on the fragment length with some optimal length which is transported most efficiently. By means of a simple one-channel model, we show that this hypothesis can explain both the one- and the three-peak length distributions found in experiments. A possible mechanism of such translocation is provided by so-called fluctuation-driven transport. KW - proteasome KW - protein translocation KW - stochastic process KW - ratchets Y1 - 2006 U6 - https://doi.org/10.1007/s10867-006-9014-z SN - 0092-0606 VL - 32 IS - 3-4 SP - 231 EP - 243 PB - Springer CY - Dordrecht ER - TY - JOUR A1 - Diercke, Andrea A1 - Kuckein, Christoph A1 - Denker, Carsten T1 - Dynamics and connectivity of an extended arch filament system JF - Astronomy and astrophysics : an international weekly journal N2 - Aims. In this study, we analyzed a filament system, which expanded between moving magnetic features (MMFs) of a decaying sunspot and opposite flux outside of the active region from the nearby quiet-Sun network. This configuration deviated from a classical arch filament system (AFS), which typically connects two pores in an emerging flux region. Thus, we called this system an extended AFS. We contrasted classical and extended AFSs with an emphasis on the complex magnetic structure of the latter. Furthermore, we examined the physical properties of the extended AFS and described its dynamics and connectivity. Methods. The extended AFS was observed with two instruments at the Dunn Solar Telescope (DST). The Rapid Oscillations in the Solar Atmosphere (ROSA) imager provided images in three different wavelength regions, which covered the dynamics of the extended AFS at different atmospheric heights. The Interferometric Bidimensional Spectropolarimeter (IBIS) provided spectroscopic Ha data and spectropolarimetric data that was obtained in the near-infrared (NIR) Call lambda 8542 angstrom line. We derived the corresponding line-of-sight (LOS) velocities and used He II lambda 304 angstrom extreme ultraviolet (EUV) images of the Atmospheric Imaging Assembly (AIA) and LOS magnetograms of the Helioseismic and Magnetic Imager (HMI) on board the Solar Dynamics Observatory (SDO) as context data. Results. The NIR Call Stokes-V maps are not suitable to definitively define a clear polarity inversion line and to classify this chromospheric structure. Nevertheless, this unusual AFS connects the MMFs of a decaying sunspot with the network field. At the southern footpoint, we measured that the flux decreases over time. We find strong downflow velocities at the footpoints of the extended AFS, which increase in a time period of 30 min. The velocities are asymmetric at both footpoints with higher velocities at the southern footpoint. An EUV brigthening appears in one of the arch filaments, which migrates from the northern footpoint toward the southern one. This activation likely influences the increasing redshift at the southern footpoint. Conclusions. The extended AFS exhibits a similar morphology as classical AFSs, for example, threaded filaments of comparable length and width. Major differences concern the connection from MMFs around the sunspot with the flux of the neighboring quietSun network, converging footpoint motions, and longer lifetimes of individual arch filaments of about one hour, while the extended AFS is still very dynamic. KW - methods: observational KW - Sun: filaments, prominences KW - Sun: activity KW - techniques: image processing KW - Sun: chromosphere Y1 - 2019 U6 - https://doi.org/10.1051/0004-6361/201935583 SN - 1432-0746 VL - 629 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Saha, Sourav A1 - Owen, Lewis A. A1 - Orr, Elizabeth N. A1 - Caffee, Marc W. T1 - High-frequency Holocene glacier fluctuations in the Himalayan-Tibetan orogen JF - Quaternary science reviews : the international multidisciplinary research and review journal N2 - Holocene glacial chronostratigraphies in glaciated valleys spread throughout the Himalayan-Tibetan orogen, including the Himalaya, Tibet, Pamir, and Tian Shan, are developed using a landsystems approach, detailed geomorphic mapping, and new and published Be-10 surface exposure dating. New studies in the Kulti valley of Lahul and the Parkachik valley of the Nun Kun massif of the Himalaya of northern India define three glacier advances at similar to 14.7, 12.2, 0.5 ka, in addition to one historically dated late 19th Century advance in the Kulti valley, and one Late Holocene advance at similar to 0.2 ka in the Parkachik valley. Three major climatic groups (subdivided into five climatic zones) are defined across the orogen using Cluster Analysis (CA) and Principal Component Analysis (PCA) to identify glaciated regions with comparable climatic characteristics to evaluate the timing, and extent of Holocene glacier advances across these regions. Our regional analyses across the Himalayan-Tibetan orogen suggest at least one Lateglacial (similar to 15.3-11.8 ka) and five Himalayan-Tibetan Holocene glacial stages (HTHS) at similar to 11.5-9.5, similar to 8.8-7.7, similar to 7.0-3.2, similar to 2.3-1.0, and <1 ka. The extent (amplitude) of glacier advances in 77 glaciated valleys is reconstructed and defined using equilibrium-line altitudes (ELAs). Modern glacier hypsometries are also assessed to help explain the intra-regional variations in glacier amplitudes during each regional glacier advance. A linear inverse glacier flow model is used to decipher the net changes in temperature (Delta T) between periods of reconstructed regional glacier advances in 66 glaciated valleys across different climatic regions throughout the orogen. The Be-10, ELAs, and Delta T data suggest enhanced monsoonal and increased precipitation during the Early Holocene, followed by relative cooling and increased aridity during the Mid- and Late Holocene that influenced glaciation. The sublimation-dominated cold-based glaciers in the northern regions of Himalayan-Tibetan orogen are more affected during these shifts in climate than the temperate glaciers in the south. (C) 2019 Elsevier Ltd. All rights reserved. KW - Holocene KW - Glaciation Central Asia KW - Cosmogenic isotopes KW - Paleoclimate modeling KW - Equilibrium-line altitudes Y1 - 2019 U6 - https://doi.org/10.1016/j.quascirev.2019.07.021 SN - 0277-3791 VL - 220 SP - 372 EP - 400 PB - Elsevier CY - Oxford ER - TY - JOUR A1 - Liu, Ruo-Yu A1 - Yan, Huirong A1 - Zhang, Heshou T1 - Role of Anisotropic Diffusion of Particles JF - Physical review letters N2 - In this Letter, we propose that the x-ray and the TeV observations in the vicinity of Geminga can be understood in the framework of anisotropic diffusion of injected electrons or positrons. This interpretation only requires the turbulence in the vicinity of Geminga to be sub-Alfvenic with the local mean magnetic field direction approximately aligned with our line of sight towards Geminga, without invoking extreme conditions for the environment, such as an extremely small diffusion coefficient and a weak magnetic field of submicrogauss as suggested in previous literature. Y1 - 2019 U6 - https://doi.org/10.1103/PhysRevLett.123.221103 SN - 0031-9007 SN - 1079-7114 VL - 123 IS - 22 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Lever, Fabiano A1 - Ramelow, Sven A1 - Gühr, Markus T1 - Effects of time-energy correlation strength in molecular entangled photon spectroscopy JF - Physical review : A, Atomic, molecular, and optical physics N2 - In this paper, we explore the time-energy domain quantum-classical transition comparing a classical pump-probe experiment on a diatomic molecule to its quantum enhanced counterpart, where the pump and probe pulses are substituted by the signal and idler beams of a spontaneous parametric down conversion (SPDC) source. Absorption of biphotons generated with SPDC exploits quantum time-energy entanglement to enhance the overall yield and selectivity of the process, when compared with a classical pump-probe setup, while maintaining femtosecond time resolution. We systematically study the effects of correlation strength on process efficiency and selectivity, comparing the results to classical pump-probe spectra. An excitation scheme to improve the yield based on spectral narrowing of biphotons is shown. The results indicate that the quantum improvements in yield are caused by a more efficient use of the total power available for the process. Y1 - 2019 U6 - https://doi.org/10.1103/PhysRevA.100.053844 SN - 2469-9926 SN - 2469-9934 VL - 100 IS - 5 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Berrah, N. A1 - Sánchez-González, Álvaro A1 - Jurek, Zoltan A1 - Obaid, Razib A1 - Xiong, H. A1 - Squibb, R. J. A1 - Osipov, T. A1 - Lutman, A. A1 - Fang, L. A1 - Barillot, T. A1 - Bozek, J. D. A1 - Cryan, J. A1 - Wolf, T. J. A. A1 - Rolles, Daniel A1 - Coffee, R. A1 - Schnorr, Kirsten A1 - Augustin, S. A1 - Fukuzawa, Hironobu A1 - Motomura, K. A1 - Niebuhr, Nina Isabelle A1 - Frasinski, L. J. A1 - Feifel, Raimund A1 - Schulz, Claus-Peter A1 - Toyota, Kenji A1 - Son, Sang-Kil A1 - Ueda, K. A1 - Pfeifer, T. A1 - Marangos, J. P. A1 - Santra, Robin T1 - Femtosecond-resolved observation of the fragmentation of buckminsterfullerene following X-ray multiphoton ionization JF - Nature physics N2 - X-ray free-electron lasers have, over the past decade, opened up the possibility of understanding the ultrafast response of matter to intense X-ray pulses. In earlier research on atoms and small molecules, new aspects of this response were uncovered, such as rapid sequences of inner-shell photoionization and Auger ionization. Here, we studied a larger molecule, buckminsterfullerene (C-60), exposed to 640 eV X-rays, and examined the role of chemical effects, such as chemical bonds and charge transfer, on the fragmentation following multiple ionization of the molecule. To provide time resolution, we performed femtosecond-resolved X-ray pump/X-ray probe measurements, which were accompanied by advanced simulations. The simulations and experiment reveal that despite substantial ionization induced by the ultrashort (20 fs) X-ray pump pulse, the fragmentation of C-60 is considerably delayed. This work uncovers the persistence of the molecular structure of C-60, which hinders fragmentation over a timescale of hundreds of femtoseconds. Furthermore, we demonstrate that a substantial fraction of the ejected fragments are neutral carbon atoms. These findings provide insights into X-ray free-electron laser-induced radiation damage in large molecules, including biomolecules. Y1 - 2019 U6 - https://doi.org/10.1038/s41567-019-0665-7 SN - 1745-2473 SN - 1745-2481 VL - 15 IS - 12 SP - 1279 EP - 1301 PB - Nature Publ. Group CY - London ER - TY - JOUR A1 - Rüdiger, Günther A1 - Schultz, M. T1 - Non-diffusive angular momentum transport in rotating z-pinches JF - Journal of plasma physics N2 - The stability of conducting Taylor-Couette flows under the presence of toroidal magnetic background fields is considered. For strong enough magnetic amplitudes such magnetohydrodynamic flows are unstable against non-axisymmetric perturbations which may also transport angular momentum. In accordance with the often used diffusion approximation, one expects the angular momentum transport to be vanishing for rigid rotation. In the sense of a non-diffusive Lambda effect, however, even for rigidly rotating z-pinches, an axisymmetric angular momentum flux appears which is directed outward (inward) for large (small) magnetic Mach numbers. The internal rotation in a magnetized rotating tank can thus never be uniform. Those particular rotation laws are used to estimate the value of the instability-induced eddy viscosity for which the non-diffusive Lambda effect and the diffusive shear-induced transport compensate each other. The results provide the Shakura & Sunyaev viscosity ansatz leading to numerical values linearly growing with the applied magnetic field. KW - plasma instabilities KW - astrophysical plasmas Y1 - 2019 U6 - https://doi.org/10.1017/S0022377819000606 SN - 0022-3778 SN - 1469-7807 VL - 85 IS - 6 PB - Cambridge Univ. Press CY - New York ER - TY - JOUR A1 - Schroetter, Ilane A1 - Bouche, Nicolas F. A1 - Zabl, Johannes A1 - Contini, Thierry A1 - Wendt, Martin A1 - Schaye, Joop A1 - Mitchell, Peter A1 - Muzahid, Sowgat A1 - Marino, Raffaella Anna A1 - Bacon, Roland A1 - Lilly, Simon J. A1 - Richard, Johan A1 - Wisotzki, Lutz T1 - MusE GAs FLOw andWind (MEGAFLOW) BT - III. Galactic wind properties using background quasars JF - Monthly notices of the Royal Astronomical Society N2 - We present results from our on-going MusE GAs FLOw and Wind (MEGAFLOW) survey, which consists of 22 quasar lines of sight, each observed with the integral field unit MUSE and the UVES spectrograph at the ESO Very Large Telescopes (VLT). The goals of this survey are to study the properties of the circumgalactic medium around z similar to 1 star-forming galaxies. The absorption-line selected survey consists of 79 strong MgII absorbers (with rest-frame equivalent width greater than or similar to 0.3 angstrom) and, currently, 86 associated galaxies within 100 projected kpc of the quasar with stellar masses (M-star) from 109 to 1011 M-circle dot. We find that the cool halo gas traced by MgII is not isotropically distributed around these galaxies from the strong bi-modal distribution in the azimuthal angle of the apparent location of the quasar with respect to the galaxy major axis. This supports a scenario in which outflows are bi-conical in nature and co-exist with a co-planar gaseous structure extending at least up to 60-80 kpc. Assuming that absorbers near the minor axis probe outflows, the current MEGAFLOW sample allowed us to select 26 galaxy-quasar pairs suitable for studying winds. From this sample, using a simple geometrical model, we find that the outflow velocity only exceeds the escape velocity when M-star less than or similar to 4 x 10(9) M-circle dot, implying the cool material is likely to fall back except in the smallest haloes. Finally, we find that the mass loading factor., the ratio between the ejected mass rate and the star formation rate, appears to be roughly constant with respect to the galaxy mass. KW - galaxies: evolution KW - galaxies: formation KW - intergalactic medium KW - quasars: absorption lines Y1 - 2019 U6 - https://doi.org/10.1093/mnras/stz2822 SN - 0035-8711 SN - 1365-2966 VL - 490 IS - 3 SP - 4368 EP - 4381 PB - Oxford Univ. Press CY - Oxford ER - TY - GEN A1 - Goychuk, Igor T1 - Comment on "Anomalous Escape Governed by Thermal 1/f Noise" Reply (R. K. Singh) T2 - Physical review letters Y1 - 2019 U6 - https://doi.org/10.1103/PhysRevLett.123.238902 SN - 0031-9007 SN - 1079-7114 VL - 123 IS - 23 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Petitgirard, Sylvain A1 - Spiekermann, Georg A1 - Glazyrin, Konstantin A1 - Garrevoet, Jan A1 - Murakami, Motohiko T1 - Density of amorphous GeO2 to 133 GPa with possible pyritelike structure and stiffness at high pressure JF - Physical review : B, Condensed matter and materials physics N2 - Germanium oxide is a prototype network-forming oxide with pressure-induced structural changes similar to those found in crystals and amorphous silicate oxides at high pressure. Studying density and coordination changes in amorphous GeO2 allows for insight into structural changes in silicate oxides at very high pressure, with implications for the properties of planetary magmas. Here, we report the density of germanium oxide glass up to 133 GPa using the x-ray absorption technique, with very good agreement with previous experimental data at pressure below 40 GPa and recent calculation up to 140 GPa. Our data highlight four distinct compressibility domains, corresponding to changes of the local structure of GeO2. Above 80 GPa, our density data show a compressibility and bulk modulus similar to the counterpart crystal phase, and we propose that a compact distorted sixfold coordination, similar to the structural motif of the pyritelike crystalline GeO2 polymorph, is likely to be stable in that pressure range. Our density data point to a smooth continuous evolution of the average coordination for pressure above 20 GPa with persistent sixfold coordination, without sharp density or density slope discontinuities. These observations are in very good agreement with theoretical calculations and spectroscopic measurements, and our results indicate that glasses and melts may behave similarly to their high-pressure solid counterparts with comparable densities, compressibility, and possibly average coordination. Y1 - 2019 U6 - https://doi.org/10.1103/PhysRevB.100.214104 SN - 2469-9950 SN - 2469-9969 VL - 100 IS - 21 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Krapf, Diego A1 - Metzler, Ralf T1 - Strange interfacial molecular dynamics JF - Physics today Y1 - 2019 U6 - https://doi.org/10.1063/PT.3.4294 SN - 0031-9228 SN - 1945-0699 VL - 72 IS - 9 SP - 48 EP - 54 PB - American Institute of Physics CY - Melville ER - TY - JOUR A1 - Teichmann, Erik A1 - Rosenblum, Michael T1 - Solitary states and partial synchrony in oscillatory ensembles with attractive and repulsive interactions JF - Chaos : an interdisciplinary journal of nonlinear science N2 - We numerically and analytically analyze transitions between different synchronous states in a network of globally coupled phase oscillators with attractive and repulsive interactions. The elements within the attractive or repulsive group are identical, but natural frequencies of the groups differ. In addition to a synchronous two-cluster state, the system exhibits a solitary state, when a single oscillator leaves the cluster of repulsive elements, as well as partially synchronous quasiperiodic dynamics. We demonstrate how the transitions between these states occur when the repulsion starts to prevail over attraction. Y1 - 2019 U6 - https://doi.org/10.1063/1.5118843 SN - 1054-1500 SN - 1089-7682 VL - 29 IS - 9 PB - American Institute of Physics CY - Melville ER - TY - GEN A1 - Cestnik, Rok A1 - Abel, Markus T1 - Erratum: Inferring the dynamics of oscillatory systems using recurrent neural networks (Chaos : an interdisciplinary journal of nonlinear science. - 29 (2019) 063128) T2 - Chaos : an interdisciplinary journal of nonlinear science Y1 - 2019 U6 - https://doi.org/10.1063/1.5122803 SN - 1054-1500 SN - 1089-7682 VL - 29 IS - 8 PB - American Institute of Physics CY - Melville ER - TY - JOUR A1 - Meyer, Dominique M.-A. A1 - Kreplin, Alexander A1 - Kraus, S. A1 - Vorobyov, E. I. A1 - Haemmerlé, Lionel A1 - Eislöffel, Jochen T1 - On the ALMA observability of nascent massive multiple systems formed by gravitational instability JF - Monthly notices of the Royal Astronomical Society N2 - Massive young stellar objects (MYSOs) form during the collapse of high-mass pre-stellar cores, where infalling molecular material is accreted through a centrifugally balanced accretion disc that is subject to efficient gravitational instabilities. In the resulting fragmented accretion disc of the MYSO, gaseous clumps and low-mass stellar companions can form, which will influence the future evolution of massive protostars in the Hertzsprung-Russell diagram. We perform dust continuum radiative transfer calculations and compute synthetic images of disc structures modelled by the gravito-radiation-hydrodynamics simulation of a forming MYSO, in order to investigate the Atacama Large Millimeter/submillimeter Array (alma) observability of circumstellar gaseous clumps and forming multiple systems. Both spiral arms and gaseous clumps located at similar or equal to a few from the protostar can be resolved by interferometric alma Cycle 7 C43-8 and C43-10 observations at band 6 (), using a maximal 0.015 aracsec beam angular resolution and at least exposure time for sources at distances of . Our study shows that substructures are observable regardless of their viewing geometry or can be inferred in the case of an edge-viewed disc. The observation probability of the clumps increases with the gradually increasing efficiency of gravitational instability at work as the disc evolves. As a consequence, large discs around MYSOs close to the zero-age-main-sequence line exhibit more substructures than at the end of the gravitational collapse. Our results motivate further observational campaigns devoted to the close surroundings of the massive protostars S255IR-NIRS3 and NGC 6334I-MM1, whose recent outbursts are a probable signature of disc fragmentation and accretion variability. KW - radiative transfer KW - methods: numerical KW - stars: circumstellar matter Y1 - 2019 U6 - https://doi.org/10.1093/mnras/stz1585 SN - 0035-8711 SN - 1365-2966 VL - 487 IS - 4 SP - 4473 EP - 4491 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Niven, Robert K. A1 - Abel, Markus A1 - Schlegel, Michael A1 - Waldrip, Steven H. T1 - Maximum Entropy Analysis of Flow Networks: Theoretical Foundation and Applications JF - Entropy N2 - The concept of a "flow network"-a set of nodes and links which carries one or more flows-unites many different disciplines, including pipe flow, fluid flow, electrical, chemical reaction, ecological, epidemiological, neurological, communications, transportation, financial, economic and human social networks. This Feature Paper presents a generalized maximum entropy framework to infer the state of a flow network, including its flow rates and other properties, in probabilistic form. In this method, the network uncertainty is represented by a joint probability function over its unknowns, subject to all that is known. This gives a relative entropy function which is maximized, subject to the constraints, to determine the most probable or most representative state of the network. The constraints can include "observable" constraints on various parameters, "physical" constraints such as conservation laws and frictional properties, and "graphical" constraints arising from uncertainty in the network structure itself. Since the method is probabilistic, it enables the prediction of network properties when there is insufficient information to obtain a deterministic solution. The derived framework can incorporate nonlinear constraints or nonlinear interdependencies between variables, at the cost of requiring numerical solution. The theoretical foundations of the method are first presented, followed by its application to a variety of flow networks. KW - maximum entropy analysis KW - flow network KW - probabilistic inference Y1 - 2019 U6 - https://doi.org/10.3390/e21080776 SN - 1099-4300 VL - 21 IS - 8 SP - 776 PB - MDPI CY - Basel ER - TY - JOUR A1 - Seiler, Michael A1 - Seiß, Martin A1 - Hoffmann, Holger A1 - Spahn, Frank T1 - Hydrodynamic Simulations of Asymmetric Propeller Structures in Saturn's Rings JF - The astrophysical journal : an international review of spectroscopy and astronomical physics ; Supplement series N2 - The observation of the non-Keplerian behavior of propeller structures in Saturn's outer A ring raises the question: how does the propeller respond to the wandering of the central embedded moonlet? Here, we study numerically how the structural imprint of the propeller changes for a libration of the moonlet. It turns out that the libration induces an asymmetry in the propeller, which depends on the libration period and amplitude of the moonlet. Further, we study the dependence of the asymmetry on the libration period and amplitude for a moonlet with a 400 m Hill radius, which is located in the outer A ring. This allows us to apply our findings to the largest known propeller Blériot, which is expected to be of a similar size. For Blériot, we can conclude that, supposing the moonlet is librating with the largest observed period of 11.1 yr and an azimuthal amplitude of about 1845 km, a small asymmetry should be measurable but depends on the moonlet's libration phase at the observation time. The longitude residuals of other trans-Encke propellers (e.g., Earhart) show amplitudes similar to Blériot, which might allow us to observe larger asymmetries due to their smaller azimuthal extent, allowing us to scan the whole gap structure for asymmetries in one observation. Although the librational model of the moonlet is a simplification, our results are a first step toward the development of a consistent model for the description of the formation of asymmetric propellers caused by a freely moving moonlet. KW - Hydrodynamics KW - methods: data analysis KW - methods: numerical KW - planets and satellites: dynamical evolution and stability KW - planets and satellites: individual (Saturn) KW - planets and satellites: rings Y1 - 2019 U6 - https://doi.org/10.3847/1538-4365/ab26b0 SN - 0067-0049 SN - 1538-4365 VL - 243 IS - 2 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Richter, Lothar A1 - Vollhardt, Dieter T1 - Force measuring methods for determination of surface tension of liquids: A comparison JF - Tenside, surfactants, detergents N2 - Three methods for the determination of the surface tension of liquids based on force measurements namely, the vertical plate method of Wilhelmy, the frame method of Lenard and the ring method of du Nouy are compared and studied in respect of a common principle of correction. It is shown that these three most important force-based methods allow the determination of the surface tension under static conditions. The force components of the corresponding liquid column below the measuring wire obtained for the straight part of the withdrawal curve up to the transition in its curved part provides exact surface tension values. The experimentally accessible value of the force component describes the physical background of the measured value correction contrary to the approximate equations obtained by mathematical way. Usually the determination of surface tension of liquids is based merely at the vertical plate method on exact equations thermodynamically derived whereas in the case of the frame and ring methods correction factors in approximate equations are used. At usual application of the force-based methods under the non-static condition of the withdrawal of a liquid column, the force maximum measured at withdrawal of the measuring object (plate, frame, or ring) is the basis for the determination of surface tension. In these cases, the measured surface tension values are compensated by correction equations for the frame and ring methods which are based on an correction factor and correction tables empirically obtained. The surface tension values obtained in this usual way agree with those obtained by using the force component of the corresponding liquid column below the measuring wire for the straight part of the withdrawal curve up to the transition in its curved part. Problems arising at the force measurements with increasing thickness of the measuring wires inside and outside the rings are discussed. N2 - Drei auf Kraftmessungen basierende Methoden zur Bestimmung der Oberflächenspannung von Flüssigkeiten, nämlich die Vertikalplattenmethode von Wilhelmy, die Bügelmethode von Lenard und die Ringmethode von du Noüy werden miteinander verglichen und auf ein experimentell zugängliches gemeinsames Korrekturprinzip hin untersucht. Auf Basis der Messresultate wird demonstriert, dass diese drei wichtigsten auf Kraftmessungen basierenden Methoden eine exakte Bestimmung der Oberflächenspannung ermöglichen. Dies basiert auf Berücksichtigung der Kraftkomponente der entsprechenden Flüssigkeitssäule unterhalb des Messdrahtes, der für die Austauchgerade bis zum Übergang in den gekrümmten Teil der Austauchkurve erhalten wird. Der experimentell zugängliche Wert der Kraftkomponente beschreibt den physikalischen Hintergrund der Messwertkorrektur im Gegensatz zu den auf mathematischen Weg erhaltenen Näherungsgleichungen. Gebräuchlicher Weise basiert die Bestimmung der Oberflächenspannung von Flüssigkeiten lediglich bei der Vertikalplattenmethode auf thermodynamisch-exakt ableitbaren Gleichungen, während bei Bügel- und Ringmethode Korrekturfaktoren für Näherungsgleichungen bzw. Korrekturtabellen üblich sind. Die so erhaltenen Oberflächenspannungswerte stimmen mit denen überein, die unter Berücksichtigung der Kraftkomponente der entsprechenden Flüssigkeitssäule unterhalb des Messdrahtes erhalten werden. Probleme, die mit zunehmender Dicke des Messdrahtes innerhalb und außerhalb des Rings entstehen, werden diskutiert. T2 - Kraftmessungsmethoden zur Bestimmung der Oberflächenspannung von Flüssigkeiten: Ein Vergleich KW - surface tension KW - force methods Y1 - 2006 U6 - https://doi.org/10.3139/113.100314 SN - 0932-3414 VL - 43 IS - 5 SP - 256 EP - 261 PB - Hanser CY - München ER - TY - JOUR A1 - Assmann, Birte A1 - Thiel, Marco A1 - Romano, Maria Carmen A1 - Niemitz, Carsten T1 - Recurrence plot analyses suggest a novel reference system involved in newborn spontaneous movements JF - Behavior research methods : a journal of the Psychonomic Society N2 - The movements of newborns have been thoroughly studied in terms of reflexes, muscle synergies, leg coordination, and target-directed arm/hand movements. Since these approaches have concentrated mainly on separate accomplishments, there has remained a clear need for more integrated investigations. Here, we report an inquiry in which we explicitly concentrated on taking such a perspective and, additionally, were guided by the methodological concept of home base behavior, which Ilan Golard developed for studies of exploratory behavior in animals. Methods from nonlinear dynamics, such as symbolic dynamics and recurrence plot analyses of kinematic data received from audiovisual newborn recordings, yielded new insights into the spatial and temporal organization of limb movements. In the framework of home base behavior, our approach uncovered a novel reference system of spontaneous newborn movements. Y1 - 2006 U6 - https://doi.org/10.3758/BF03192793 SN - 1554-351X SN - 1554-3528 VL - 38 IS - 3 SP - 400 EP - 406 PB - Springer CY - New York ER - TY - JOUR A1 - Diez, Isabel A1 - Tauer, Klaus A1 - Schulz, Burkhard T1 - Unusual polymer dispersions-polypyrrole suspensions made of rings, frames, and platelets JF - Colloid and polymer science : official journal of the Kolloid-Gesellschaft N2 - Experimental results show that the polymerization of pyrrole in the presence of beta-naphthalenesulfonic acid and different fluorosurfactants like perfluorooctanesulfonic acid, perfluorooctyldiethanolamide, and ammonium perfluorooctanoate leads to polypyrrole with special morphologies, such as rings or disks and rectangular frames or plates. The formation of these unusually shaped particles of polymer dispersions is explained by the chemical and colloidal peculiarities of the oxidative pyrrole polymerization with ammonium peroxodisulfate in aqueous medium. KW - polypyrrole KW - chemical oxidative polymerization KW - particle morphology Y1 - 2006 U6 - https://doi.org/10.1007/s00396-006-1521-8 SN - 0303-402X VL - 284 SP - 1431 EP - 1442 PB - Springer CY - New York ER - TY - JOUR A1 - Giesers, Benjamin David A1 - Kamann, Sebastian A1 - Dreizler, Stefan A1 - Husser, Tim-Oliver A1 - Askar, Abbas A1 - Göttgens, Fabian A1 - Brinchmann, Jarle A1 - Latour, Marilyn A1 - Weilbacher, Peter Michael A1 - Wendt, Martin A1 - Roth, Martin M. T1 - A stellar census in globular clusters with MUSE: Binaries in NGC 3201 JF - Astronomy and astrophysics : an international weekly journal N2 - We utilise multi-epoch MUSE spectroscopy to study binary stars in the core of the Galactic globular cluster NGC 3201. Our sample consists of 3553 stars with 54 883 spectra in total comprising 3200 main-sequence stars up to 4 magnitudes below the turn-off. Each star in our sample has between 3 and 63 (with a median of 14) reliable radial velocity measurements within five years of observations. We introduce a statistical method to determine the probability of a star showing radial velocity variations based on the whole inhomogeneous radial velocity sample. Using HST photometry and an advanced dynamical MOCCA simulation of this specific cluster we overcome observational biases that previous spectroscopic studies had to deal with. This allows us to infer a binary frequency in the MUSE field of view and enables us to deduce the underlying true binary frequency of (6.75 +/- 0.72)% in NGC 3201. The comparison of the MUSE observations with the MOCCA simulation suggests a large portion of primordial binaries. We can also confirm a radial increase in the binary fraction towards the cluster centre due to mass segregation. We discovered that in the core of NGC 3201 at least (57.5 +/- 7.9)% of blue straggler stars are in a binary system. For the first time in a study of globular clusters, we were able to fit Keplerian orbits to a significant sample of 95 binaries. We present the binary system properties of eleven blue straggler stars and the connection to SX Phoenicis-type stars. We show evidence that two blue straggler formation scenarios, the mass transfer in binary (or triple) star systems and the coalescence due to binary-binary interactions, are present in our data. We also describe the binary and spectroscopic properties of four sub-subgiant (or red straggler) stars. Furthermore, we discovered two new black hole candidates with minimum masses (M sin i) of (7.68 +/- 0.50)M-circle dot, (4.4 +/- 2.8)M-circle dot, and refine the minimum mass estimate on the already published black hole to (4.53 +/- 0.21)M-circle dot, These black holes are consistent with an extensive black hole subsystem hosted by NGC 3201. KW - binaries: general KW - blue stragglers KW - stars: black holes KW - techniques: radial velocities KW - techniques: imaging spectroscopy KW - globular clusters: individual: NGC 3201 Y1 - 2019 U6 - https://doi.org/10.1051/0004-6361/201936203 SN - 0004-6361 SN - 1432-0746 VL - 632 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Latour, Marlyn A1 - Husser, Tim Oliver A1 - Giesers, Benjamin David A1 - Kamann, S. A1 - Göttgens, Fabian A1 - Dreizler, Stefan A1 - Brinchmann, Jan A1 - Bastian, Nate A1 - Wendt, Martin A1 - Weilbacher, Peter Michael A1 - Molinski, N. S. T1 - A stellar census in globular clusters with MUSE: multiple populations chemistry in NGC 2808 star star star JF - Astronomy and astrophysics : an international weekly journal N2 - Context. Galactic globular clusters (GCs) are now known to host multiple populations displaying particular abundance variations. The different populations within a GC can be well distinguished following their position in the pseudo two-colors diagrams, also referred to as "chromosome maps". These maps are constructed using optical and near-UV photometry available from the Hubble Space Telescope (HST) UV survey of GCs. However, the chemical tagging of the various populations in the chromosome maps is hampered by the fact that HST photometry and elemental abundances are both only available for a limited number of stars. Aims. The spectra collected as part of the MUSE survey of globular clusters provide a spectroscopic counterpart to the HST photometric catalogs covering the central regions of GCs. In this paper, we use the MUSE spectra of 1115 red giant branch (RGB) stars in NGC 2808 to characterize the abundance variations seen in the multiple populations of this cluster. Methods. We used the chromosome map of NGC 2808 to divide the RGB stars into their respective populations. We then combined the spectra of all stars belonging to a given population, resulting in one high signal-to-noise ratio spectrum representative of each population. Results. Variations in the spectral lines of O, Na, Mg, and Al are clearly detected among four of the populations. In order to quantify these variations, we measured equivalent width differences and created synthetic populations spectra that were used to determine abundance variations with respect to the primordial population of the cluster. Our results are in good agreement with the values expected from previous studies based on high-resolution spectroscopy. We do not see any significant variations in the spectral lines of Ca, K, and Ba. We also do not detect abundance variations among the stars belonging to the primordial population of NGC 2808. Conclusions. We demonstrate that in spite of their low resolution, the MUSE spectra can be used to investigate abundance variations in the context of multiple populations. KW - techniques: imaging spectroscopy KW - stars: abundances KW - globular clusters: individual: NGC 2808 Y1 - 2019 U6 - https://doi.org/10.1051/0004-6361/201936242 SN - 1432-0746 VL - 631 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Fox, Andrew J. A1 - Richter, Philipp A1 - Ashley, Trisha A1 - Heckman, Timothy M. A1 - Lehner, Nicolas A1 - Werk, Jessica K. A1 - Bordoloi, Rongmon A1 - Peeples, Molly S. T1 - The Mass Inflow and Outflow Rates of the Milky Way JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - We present new calculations of the mass inflow and outflow rates around the Milky Way (MW), derived from a catalog of ultraviolet metal-line high-velocity clouds (HVCs). These calculations are conducted by transforming the HVC velocities into the Galactic standard of rest (GSR) reference frame, identifying inflowing (vGSR.<.0 km s(-1)) and outflowing (vGSR > 0 km s(-1)) populations, and using observational constraints on the distance, metallicity, dust content, covering fractions, and total silicon column density of each population. After removing HVCs associated with the Magellanic Stream and the Fermi Bubbles, we find inflow and outflow rates in cool (T similar to 10(4) K) ionized gas of dM(in)/dt greater than or similar to.(0.53 +/- 0.23)(d/12 kpc)(Z/0.2Z(circle dot))-1M(circle dot) yr(-1) and dM(out)/dt greater than or similar to (0.16 +/- 0.07)(d/12 kpc)(Z/0.5Z(circle dot))M--1(circle dot) yr(-1). The apparent excess of inflowing over outflowing gas suggests that the MW is currently in an inflow-dominated phase, but the presence of substantial mass flux in both directions supports a Galactic fountain model, in which gas is constantly recycled between the disk and the halo. We also find that the metal flux in both directions (in and out) is indistinguishable. By comparing the outflow rate to the Galactic star formation rate, we present the first estimate of the mass loading factor (eta(HVC)) of the disk-wide MW wind, finding eta(HVC) greater than or similar to (0.10 +/- 0.06)(d/12 kpc)(Z/0.5Z(circle dot))(-1). Including the contributions from low- and intermediatevelocity clouds and from hot gas would increase these inflow and outflow estimates. Y1 - 2019 U6 - https://doi.org/10.3847/1538-4357/ab40ad SN - 0004-637X SN - 1538-4357 VL - 884 IS - 1 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Mei, Shilin A1 - Kochovski, Zdravko A1 - Roa, Rafael A1 - Gu, Sasa A1 - Xu, Xiaohui A1 - Yu, Hongtao A1 - Dzubiella, Joachim A1 - Ballauff, Matthias A1 - Lu, Yan T1 - Enhanced Catalytic Activity of Gold@Polydopamine Nanoreactors with Multi-compartment Structure Under NIR Irradiation JF - Nano-Micro Letters N2 - Photothermal conversion (PTC) nanostructures have great potential for applications in many fields, and therefore, they have attracted tremendous attention. However, the construction of a PTC nanoreactor with multi-compartment structure to achieve the combination of unique chemical properties and structural feature is still challenging due to the synthetic difficulties. Herein, we designed and synthesized a catalytically active, PTC gold (Au)@polydopamine (PDA) nanoreactor driven by infrared irradiation using assembled PS-b-P2VP nanosphere as soft template. The particles exhibit multi-compartment structure which is revealed by 3D electron tomography characterization technique. They feature permeable shells with tunable shell thickness. Full kinetics for the reduction reaction of 4-nitrophenol has been investigated using these particles as nanoreactors and compared with other reported systems. Notably, a remarkable acceleration of the catalytic reaction upon near-infrared irradiation is demonstrated, which reveals for the first time the importance of the synergistic effect of photothermal conversion and complex inner structure to the kinetics of the catalytic reduction. The ease of synthesis and fresh insights into catalysis will promote a new platform for novel nanoreactor studies. KW - Gold@polydopamine KW - 3D tomography KW - Nanoreactor KW - Catalysis KW - Photothermal conversion Y1 - 2019 U6 - https://doi.org/10.1007/s40820-019-0314-9 SN - 2311-6706 SN - 2150-5551 VL - 11 IS - 1 PB - Shanghai JIAO TONG univ press CY - Shanghai ER - TY - JOUR A1 - Saha, Sourav A1 - Owen, Lewis A. A1 - Orr, Elizabeth N. A1 - Caffee, Marc W. T1 - Cosmogenic Be-10 and equilibrium-line altitude dataset of Holocene glacier advances in the Himalayan-Tibetan orogen JF - Data in brief N2 - A comprehensive analysis of the variable temporal and spatial responses of tropical-subtropical high-altitude glaciers to climate change is critical for successful model predictions and environmental risk assessment in the Himalayan-Tibetan orogen. High-frequency Holocene glacier chronostratigraphies are therefore reconstructed in 79 glaciated valleys across the orogen using 519 published and 16 new terrestrial cosmogenic 10Be exposure age dataset. Published 10Be ages are compiled only for moraine boulders (excluding bedrock ages). These ages are recalculated using the latest ICE-D production rate calibration database and the scaling scheme models. Outliers for the individual moraine are detected using the Chauvenet's criterion. In addition, past equilibrium-line altitudes (ELAs) are determined using the area-altitude (AA), area accumulation ratio (AAR), and toe-headwall accumulation ratio (THAR) methods for each glacier advance. The modern maximum elevations of lateral moraines (MELM) are also used to estimate modern ELAs and as an independent check on mean ELAs derived using the above three methods. These data may serve as an essential archive for future studies focusing on the cryospheric and environmental changes in the Himalayan-Tibetan orogen. A more comprehensive analysis of the published and new 10Be ages and ELA results and a list of references are presented in Saha et al. (2019, High-frequency Holocene glacier fluctuations in the Himalayan-Tibetan orogen. Quaternary Science Reviews, 220, 372–400). KW - Cosmogenic nuclides KW - Equilibrium-line altitudes KW - Holocene KW - Central asia KW - Glaciation Y1 - 2019 U6 - https://doi.org/10.1016/j.dib.2019.104412 SN - 2352-3409 VL - 26 PB - Elsevier CY - Amsterdam ER - TY - JOUR A1 - Teomy, Eial A1 - Metzler, Ralf T1 - Transport in exclusion processes with one-step memory: density dependence and optimal acceleration JF - Journal of physics : A, Mathematical and theoretical N2 - We study a lattice gas of persistent walkers, in which each site is occupied by at most one particle and the direction each particle attempts to move to depends on its last step. We analyse the mean squared displacement (MSD) of the particles as a function of the particle density and their persistence (the tendency to continue moving in the same direction). For positive persistence the MSD behaves as expected: it increases with the persistence and decreases with the density. However, for strong anti-persistence we find two different regimes, in which the dependence of the MSD on the density is non-monotonic. For very strong anti-persistence there is an optimal density at which the MSD reaches a maximum. In an intermediate regime, the MSD as a function of the density exhibits both a minimum and a maximum, a phenomenon which has not been observed before. We derive a mean-field theory which qualitatively explains this behaviour. KW - exclusion process KW - persistence KW - lattice gas Y1 - 2019 U6 - https://doi.org/10.1088/1751-8121/ab37e4 SN - 1751-8113 SN - 1751-8121 VL - 52 IS - 38 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Palyulin, Vladimir V. A1 - Blackburn, George A1 - Lomholt, Michael A. A1 - Watkins, Nicholas W. A1 - Metzler, Ralf A1 - Klages, Rainer A1 - Chechkin, Aleksei V. T1 - First passage and first hitting times of Levy flights and Levy walks JF - New journal of physics : the open-access journal for physics N2 - For both Lévy flight and Lévy walk search processes we analyse the full distribution of first-passage and first-hitting (or first-arrival) times. These are, respectively, the times when the particle moves across a point at some given distance from its initial position for the first time, or when it lands at a given point for the first time. For Lévy motions with their propensity for long relocation events and thus the possibility to jump across a given point in space without actually hitting it ('leapovers'), these two definitions lead to significantly different results. We study the first-passage and first-hitting time distributions as functions of the Lévy stable index, highlighting the different behaviour for the cases when the first absolute moment of the jump length distribution is finite or infinite. In particular we examine the limits of short and long times. Our results will find their application in the mathematical modelling of random search processes as well as computer algorithms. KW - Levy flights KW - Levy walks KW - first-passage time KW - first-hitting time Y1 - 2019 U6 - https://doi.org/10.1088/1367-2630/ab41bb SN - 1367-2630 VL - 21 IS - 10 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Teomy, Eial A1 - Metzler, Ralf T1 - Correlations and transport in exclusion processes with general finite memory JF - Journal of statistical mechanics: theory and experiment KW - Brownian motion KW - exclusion processes Y1 - 2019 U6 - https://doi.org/10.1088/1742-5468/ab47fb SN - 1742-5468 VL - 2019 IS - 10 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Kurzke, Henning A1 - Kiethe, Jan A1 - Heuer, Axel A1 - Jechow, Andreas T1 - Frequency doubling of incoherent light from a superluminescent diode in a periodically poled lithium niobate waveguide crystal JF - Laser physics letters N2 - The amplified spontaneous emission from a superluminescent diode was frequency doubled in a periodically poled lithium niobate waveguide crystal. The temporally incoherent radiation of such a superluminescent diode is characterized by a relatively broad spectral bandwidth and thermal-like photon statistics, as the measured degree of second order coherence, g((2))(0)= 1.9 +/- 0.1, indicates. Despite the non-optimized scenario in the spectral domain, we achieve six orders of magnitude higher conversion efficiency than previously reported with truly incoherent light. This is possible by using single spatial mode radiation and quasi phase matched material with a waveguide architecture. This work is a principle step towards efficient frequency conversion of temporally incoherent radiation in one spatial mode to access wavelengths where no radiation from superluminescent diodes is available, especially with tailored quasi phase matched crystals. The frequency doubled light might find application in imaging, metrology and quantum optics experiments. KW - nonlinear frequency conversion KW - periodically poled material KW - waveguides KW - incoherent radiation Y1 - 2017 U6 - https://doi.org/10.1088/1612-202X/aa6889 SN - 1612-2011 SN - 1612-202X VL - 14 PB - IOP Publ. CY - Bristol ER - TY - THES A1 - Schmoll, Jürgen T1 - 3D-Spektrofotometrie extragalaktischer Emissionslinienobjekte N2 - Populärwissenschaftlicher Abstract: Bislang gibt es in der beobachtenden optischen Astronomie zwei verschiedene Herangehensweisen: Einerseits werden Objekte durch Kameras abbildend erfaßt, andererseits werden durch die wellenlängenabhängige Zerlegung ihres Lichtes Spektren gewonnen. Das Integral - Field - Verfahren ist eine relativ neue Technik, welche die genannten Beobachtungsmethoden vereint. Das Objektbild im Teleskopfokus wird in räumlich zerlegt und jedes Ortselement einem gemeinsamen Spektrografen zugeführt. Hierdurch wird das Objekt nicht nur zweidimensional räumlich erfaßt, sondern zusätzlich die spektrale Kompenente als dritte Dimension erhalten, weswegen das Verfahren auch als 3D-Methode bezeichnet wird. Anschaulich kann man sich das Datenresultat als eine Abbildung vorstellen, in der jeder einzelne Bildpunkt nicht mehr nur einen Intensitätswert enthält, sondern gleich ein ganzes Spektrum. Diese Technik ermöglicht es, ausgedehnte Objekte im Unterschied zu gängigen Spaltspektrografen komplett zu erfassen. Die besondere Stärke der Methode ist die Möglichkeit, die Hintergrundkontamination der unmittelbaren Umgebung des Objektes zu erfassen und in der Auswertung zu berücksichtigen. Durch diese Fähigkeit erscheint die 3D-Methode prädestiniert für den durch moderne Großteleskope erschlossenen Bereich der extragalaktischen Stellarastronomie. Die detaillierte Untersuchung aufgelöster stellare Populationen in nahegelegenen Galaxien ist erst seit kurzer Zeit dank der Fortschritte mit modernen Grossteleskopen und fortschrittlicher Instrumentierung möglich geworden. Wegen der Bedeutung für die Entstehung und Evolution von Galaxien werden diese Arbeiten zukünftig weiter an Bedeutung gewinnen. In der vorliegenden Arbeit wurde die Integral-Field-Spektroskopie an zwei planetarischen Nebeln in der nächstgelegenen großen Spiralgalaxie M31 (NGC 224) getestet, deren Helligkeiten und Koordinaten aus einer Durchmusterung vorlagen. Hierzu wurden Beobachtungen mit dem MPFS-Instrument am russischen 6m - Teleskop in Selentschuk/Kaukasus sowie mit INTEGRAL/WYFFOS am englischen William-Herschel-Teleskop auf La Palma gewonnen. Ein überraschendes Ergebnis war, daß eins der beiden Objekte falsch klassifiziert wurde. Sowohl die meßbare räumliche Ausdehnung des Objektes als auch das spektrale Erscheinungsbild schlossen die Identität mit einem planetarischen Nebel aus. Mit hoher Wahrscheinlichkeit handelt es sich um einen Supernovaüberrest, zumal im Rahmen der Fehler an gleicher Stelle eine vom Röntgensatelliten ROSAT detektierte Röntgenquelle liegt. Die in diesem Projekt verwendeten Integral-Field-Instrumente wiesen zwei verschiedene Bauweisen auf, die sich miteinander vergleichen ließen. Ein Hauptkritikpunkt der verwendeten Instrumente war ihre geringe Lichtausbeute. Die gesammelten Erfahrung fanden Eingang in das Konzept des derzeit in Potsdam in der Fertigung befindlichen 3D-Instruments PMAS (Potsdamer Multi - Apertur - Spektrophotometer), welcher zunächst für das 3.5m-Teleskop des Calar - Alto - Observatoriums in Südspanien vorgesehen ist. Um die Effizienz dieses Instrumentes zu verbessern, wurde in dieser Arbeit die Kopplung der zum Bildrasterung verwendeten Optik zu den Lichtleitfasern im Labor untersucht. Die Untersuchungen zur Maximierung von Lichtausbeute und Stabilität zeigen, daß sich die Effizienz durch Auswahl einer geeigneten Koppelmethode um etwa 20 Prozent steigern lässt. N2 - Popular scientific abstract: Currently there are two different approaches in the observational optical astronomy: On the first hand objects are imaged with cameras, on the other hand spectra are produced. The integral-field-technique is a relatively new way to combine both branches. The object image in the telecopes focus is sampled spatially and each spatial bin assigned to a spectrograph. Hence the object is not only sampled spatially but the spectral component is achieved as a third dimension, so the name 3D-Method. The result is like an image but each point consists of a whole spectrum. The use of this technique is to sample objects completely in contrast to standard slit spectroscopy. The strength of this method is to deal with high background light contamination. So the 3D method looks convincing for the new branch of extragalactic stellar astronomy with modern large telescopes. The detailled investigation of spatially resolved extragalactic populations in nearby galaxies is a rather new topic demanding newest telescopes and instrumentation. These investigations are very important in future to understand the origin and evolution of galaxies. In this thesis the Integral-Field-Spectroscopy was tested for two planetary nebulae in the Andromeda galaxy M31. Observations have been made using the MPFS on the Russian 6m telescope and the INTEGRAL/WYFFOS setup on the 4.2m WHT on La Palma. A surprising result was that one of the two objects was wrongly identified as a planetary nebula. The spatial extension and spectral details excluded this object class. With high probability this object is a supernova remnant. The integral-field-instruments used in this thesis had different technical layouts, which were to compare to each other. The main critics is the poor efficiency of both devices. The experience made was utilized to optimize the concept of the recently developed 3D-instrument PMAS (Potsdam Multi- Aperture Spectrophotometer). PMAS will be used for the 3.5 m telescope at the Calar Alto observatory. To improve efficiency, the coupling of the optical fibers used to sample the object and guide the light into the spectrograph was optimized in the laboratory. This investigations showed that an increase of the coupling efficiency by about 20 percent is possible by using immersion coupling between fibers and lenses. KW - Ortsauflösende Spektrofotometrie KW - extragalaktische Stellarastronomie KW - Integral field spectroscopy KW - extragalactic stellar astronomy Y1 - 2001 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-0000372 ER - TY - JOUR A1 - Kamann, Sebastian A1 - Husser, T. -O. A1 - Dreizler, S. A1 - Emsellem, E. A1 - Weilbacher, Peter Michael A1 - Martens, S. A1 - Bacon, R. A1 - den Brok, M. A1 - Giesers, B. A1 - Krajnovic, Davor A1 - Roth, Martin M. A1 - Wendt, Martin A1 - Wisotzki, Lutz T1 - A stellar census in globular clusters with MUSE BT - the contribution of rotation to cluster dynamics studied with 200 000 stars JF - Monthly notices of the Royal Astronomical Society N2 - This is the first of a series of papers presenting the results from our survey of 25 Galactic globular clusters with the MUSE integral-field spectrograph. In combination with our dedicated algorithm for source deblending, MUSE provides unique multiplex capabilities in crowded stellar fields and allows us to acquire samples of up to 20 000 stars within the half-light radius of each cluster. The present paper focuses on the analysis of the internal dynamics of 22 out of the 25 clusters, using about 500 000 spectra of 200 000 individual stars. Thanks to the large stellar samples per cluster, we are able to perform a detailed analysis of the central rotation and dispersion fields using both radial profiles and two-dimensional maps. The velocity dispersion profiles we derive show a good general agreement with existing radial velocity studies but typically reach closer to the cluster centres. By comparison with proper motion data, we derive or update the dynamical distance estimates to 14 clusters. Compared to previous dynamical distance estimates for 47 Tuc, our value is in much better agreement with other methods. We further find significant (>3 sigma) rotation in the majority (13/22) of our clusters. Our analysis seems to confirm earlier findings of a link between rotation and the ellipticities of globular clusters. In addition, we find a correlation between the strengths of internal rotation and the relaxation times of the clusters, suggesting that the central rotation fields are relics of the cluster formation that are gradually dissipated via two-body relaxation. KW - techniques: imaging spectroscopy KW - stars: kinematics and dynamics KW - globular clusters: general Y1 - 2017 U6 - https://doi.org/10.1093/mnras/stx2719 SN - 0035-8711 SN - 1365-2966 VL - 473 IS - 4 SP - 5591 EP - 5616 PB - Oxford Univ. Press CY - Oxford ER - TY - THES A1 - Stoll, Andreas T1 - Advanced spectroscopic instruments enabled by integrated optics N2 - The aim of this work is the study of silica Arrayed Waveguide Gratings (AWGs) in the context of applications in astronomy. The specific focus lies on the investigation of the feasibility and technology limits of customized silica AWG devices for high resolution near-infrared spectroscopy. In a series of theoretical and experimental studies, AWG devices of varying geometry, foot-print and spectral resolution are constructed, simulated using a combination of a numerical beam propagation method and Fraunhofer diffraction and fabricated devices are characterized with respect to transmission efficiency, spectral resolution and polarization sensitivity. The impact of effective index non-uniformities on the performance of high-resolution AWG devices is studied numerically. Characterization results of fabricated devices are used to extrapolate the technology limits of the silica platform. The important issues of waveguide birefringence and defocus aberration are discussed theoretically and addressed experimentally by selection of an appropriate aberration-minimizing anastigmatic AWG layout structure. The drawbacks of the anastigmatic AWG geometry are discussed theoretically. From the results of the experimental studies, it is concluded that fabrication-related phase errors and waveguide birefringence are the primary limiting factors for the growth of AWG spectral resolution. It is shown that, without post-processing, the spectral resolving power is phase-error-limited to R < 40, 000 and, in the case of unpolarized light, birefringence-limited to R < 30, 000 in the AWG devices presented in this work. Necessary measures, such as special waveguide geometries and post-fabrication phase error correction are proposed for future designs. The elimination of defocus aberration using an anastigmatic AWG geometry is successfully demonstrated in experiment. Finally, a novel, non-planar dispersive in-fibre waveguide structure is proposed, discussed and studied theoretically. N2 - Das Ziel der vorliegenden Arbeit ist die Untersuchung von Arrayed Waveguide Gratings (AWGs) auf SiO2-Basis im Kontext von Anwendungen in der Astronomie. Der besondere Fokus liegt auf der Untersuchung der Machbarkeit und der technologischen Grenzen von spezialisierten AWGs für die hochauflösende Nahinfrarot-Spektroskopie. In einer Reihe von theoretischen und experimentellen Studien werden AWGs unterschiedlicher Geometrie, Größe und spektraler Auflösung konstruiert, unter Verwendung einer numerischen Beam-Propagation-Methode (BPM) und Fraunhofer-Beugung simuliert und hinsichtlich Effizienz, spektraler Auflösung und Polarisationsempfindlichkeit charakterisiert. Der Einfluss von Variationen des effektiven Brechungsindex auf die Leistung von hochauflösenden AWGs wird numerisch untersucht. Mit hergestellten AWGs gewonnene Messergebnisse werden verwendet, um die technologischen Grenzen der SiO2-Plattform zu extrapolieren. Die relevanten Probleme der Polarisationsempfindlichkeit und der in kanonischen Rowland-Geometrien auftretenden Defokusaberration werden theoretisch diskutiert und experimentell durch die Auswahl einer geeigneten aberrationsminimierenden AWG-Struktur angegangen. Die Nachteile anastigmatischer AWGs werden theoretisch diskutiert. Aus den Ergebnissen der experimentellen Studien wird geschlossen, dass herstellungsbedingte Phasenfehler und Wellenleiter-Doppelbrechung die primären begrenzenden Faktoren für die Erhöhung der AWG-Spektralauflösung sind. Es wird gezeigt, dass das spektrale Auflösungsvermögen der in dieser Arbeit präsentierten AWGs ohne Phasenfehlerkorrektur auf R < 40, 000 und durch Doppelbrechung auf R < 30, 000 im Fall unpolarisierten Lichtes begrenzt ist. Notwendige Maßnahmen wie spezielle Wellenleitergeometrien und Phasenfehlerkorrektur nach der Herstellung werden für zukünftige AWG-Designs empfohlen. Die Eliminierung von Defokussierungsfehlern unter Verwendung einer anastigmatischen AWG-Geometrie wird erfolgreich im Experiment demonstriert. Schließlich wird eine neuartige, in eine optische Faser eingebettete, nicht-planare dispersive Wellenleiterstruktur vorgeschlagen, diskutiert und theoretisch untersucht. KW - Astrophotonics KW - Integrated spectrograph KW - planar lightwave circuit KW - arrayed waveguide grating KW - silica-on-silicon KW - Astrophotonik KW - integrierter Spektrograph KW - planare Lichtwellenleiter KW - Siliziumdioxid-auf-Silizium Y1 - 2022 ER - TY - JOUR A1 - Marschall, Raphael A1 - Skorov, Yuri A1 - Zakharov, Vladimir A1 - Rezac, Ladislav A1 - Gerig, Selina-Barbara A1 - Christou, Chariton A1 - Dadzie, S. Kokou A1 - Migliorini, Alessandra A1 - Rinaldi, Giovanna A1 - Agarwal, Jessica A1 - Vincent, Jean-Baptiste A1 - Kappel, David T1 - Cometary comae-surface links the physics of gas and dust from the surface to a spacecraft JF - Space science reviews N2 - A comet is a highly dynamic object, undergoing a permanent state of change. These changes have to be carefully classified and considered according to their intrinsic temporal and spatial scales. The Rosetta mission has, through its contiguous in-situ and remote sensing coverage of comet 67P/Churyumov-Gerasimenko (hereafter 67P) over the time span of August 2014 to September 2016, monitored the emergence, culmination, and winding down of the gas and dust comae. This provided an unprecedented data set and has spurred a large effort to connect in-situ and remote sensing measurements to the surface. In this review, we address our current understanding of cometary activity and the challenges involved when linking comae data to the surface. We give the current state of research by describing what we know about the physical processes involved from the surface to a few tens of kilometres above it with respect to the gas and dust emission from cometary nuclei. Further, we describe how complex multidimensional cometary gas and dust models have developed from the Halley encounter of 1986 to today. This includes the study of inhomogeneous outgassing and determination of the gas and dust production rates. Additionally, the different approaches used and results obtained to link coma data to the surface will be discussed. We discuss forward and inversion models and we describe the limitations of the respective approaches. The current literature suggests that there does not seem to be a single uniform process behind cometary activity. Rather, activity seems to be the consequence of a variety of erosion processes, including the sublimation of both water ice and more volatile material, but possibly also more exotic processes such as fracture and cliff erosion under thermal and mechanical stress, sub-surface heat storage, and a complex interplay of these processes. Seasons and the nucleus shape are key factors for the distribution and temporal evolution of activity and imply that the heliocentric evolution of activity can be highly individual for every comet, and generalisations can be misleading. KW - comets KW - coma KW - gas KW - dust KW - dynamics KW - modelling KW - inversion Y1 - 2020 U6 - https://doi.org/10.1007/s11214-020-00744-0 SN - 0038-6308 SN - 1572-9672 VL - 216 IS - 8 PB - Springer CY - Dordrecht ER - TY - JOUR A1 - Rousseau, Batiste A1 - Erard, Stéphane A1 - Beck, P. A1 - Quirico, Eric A1 - Schmitt, B. A1 - Brissaud, O. A1 - Montes-Hernandez, G. A1 - Capaccioni, F. A1 - Filacchione, Gianrico A1 - Bockelee-Morvan, Dominique A1 - Leyrat, C. A1 - Ciarniello, M. A1 - Raponi, Andrea A1 - Kappel, David A1 - Arnold, G. A1 - Moroz, L. V. A1 - Palomba, Ernesto A1 - Tosi, Federico T1 - Laboratory simulations of the Vis-NIR spectra of comet 67P using sub-mu m sized cosmochemical analogues JF - Icarus : international journal of solar system studies N2 - Laboratory spectral measurements of relevant analogue materials were performed in the framework of the Rosetta mission in order to explain the surface spectral properties of comet 67P. Fine powders of coal, iron sulphides, silicates and their mixtures were prepared and their spectra measured in the Vis-IR range. These spectra are compared to a reference spectrum of 67P nucleus obtained with the VIRTIS/Rosetta instrument up to 2.7 mu m, excluding the organics band centred at 3.2 mu m. The species used are known to be chemical analogues for cometary materials which could be present at the surface of 67P. Grain sizes of the powders range from tens of nanometres to hundreds of micrometres. Some of the mixtures studied here actually reach the very low reflectance level observed by VIRTIS on 67P. The best match is provided by a mixture of sub-micron coal, pyrrhotite, and silicates. Grain sizes are in agreement with the sizes of the dust particles detected by the GIADA, MIDAS and COSIMA instruments on board Rosetta. The coal used in the experiment is responsible for the spectral slope in the visible and infrared ranges. Pyrrhotite, which is strongly absorbing, is responsible for the low albedo observed in the NIR. The darkest components dominate the spectra, especially within intimate mixtures. Depending on sample preparation, pyrrhotite can coat the coal and silicate aggregates. Such coating effects can affect the spectra as much as particle size. In contrast, silicates seem to play a minor role. (c) 2017 Elsevier Inc. All rights reserved. KW - Comets KW - Comets nucleus KW - Comets composition KW - Spectroscopy KW - Experimental techniques Y1 - 2018 U6 - https://doi.org/10.1016/j.icarus.2017.10.015 SN - 0019-1035 SN - 1090-2643 VL - 306 SP - 306 EP - 318 PB - Elsevier CY - San Diego ER - TY - JOUR A1 - Hou, Ru A1 - Cherstvy, Andrey G. A1 - Metzler, Ralf A1 - Akimoto, Takuma T1 - Biased continuous-time random walks for ordinary and equilibrium cases BT - facilitation of diffusion, ergodicity breaking and ageing JF - Physical chemistry, chemical physics : a journal of European Chemical Societies N2 - We examine renewal processes with power-law waiting time distributions (WTDs) and non-zero drift via computing analytically and by computer simulations their ensemble and time averaged spreading characteristics. All possible values of the scaling exponent alpha are considered for the WTD psi(t) similar to 1/t(1+alpha). We treat continuous-time random walks (CTRWs) with 0 < alpha < 1 for which the mean waiting time diverges, and investigate the behaviour of the process for both ordinary and equilibrium CTRWs for 1 < alpha < 2 and alpha > 2. We demonstrate that in the presence of a drift CTRWs with alpha < 1 are ageing and non-ergodic in the sense of the non-equivalence of their ensemble and time averaged displacement characteristics in the limit of lag times much shorter than the trajectory length. In the sense of the equivalence of ensemble and time averages, CTRW processes with 1 < alpha < 2 are ergodic for the equilibrium and non-ergodic for the ordinary situation. Lastly, CTRW renewal processes with alpha > 2-both for the equilibrium and ordinary situation-are always ergodic. For the situations 1 < alpha < 2 and alpha > 2 the variance of the diffusion process, however, depends on the initial ensemble. For biased CTRWs with alpha > 1 we also investigate the behaviour of the ergodicity breaking parameter. In addition, we demonstrate that for biased CTRWs the Einstein relation is valid on the level of the ensemble and time averaged displacements, in the entire range of the WTD exponent alpha. Y1 - 2018 U6 - https://doi.org/10.1039/c8cp01863d SN - 1463-9076 SN - 1463-9084 VL - 20 IS - 32 SP - 20827 EP - 20848 PB - Royal Society of Chemistry CY - Cambridge ER - TY - THES A1 - Keles, Engin T1 - Atmospheric properties and dynamics of gaseous exoplanets inferred from high-resolution alkali line transmission spectroscopy N2 - The characterization of exoplanets applying high-resolution transmission spectroscopy ini- tiated a new era making it possible to trace atmospheric signature at high altitudes in exoplanet atmospheres and to determine atmospheric properties which enrich our under- standing of the formation and evolution of the solar system. In contrast to what is observed in our solar system, where gaseous planets orbit at wide orbits, Jupiter type exoplanets were detected in foreign stellar systems surrounding their host stars within few days, in close orbits, the so called hot- and ultra-hot Jupiters. The most well studied ones are HD209458b and HD189733b, which are the first exoplanets where absorption is detected in their atmospheres, namely from the alkali line sodium. For hot Jupiters, the resonant alkali lines are the atmospheric species with one of the strongest absorption signatures, due to their large absorption cross-section. However, al- though the alkali lines sodium and potassium were detected in low-resolution observations for various giant exoplanets, potassium was absent in different high-resolution investiga- tions in contrast to sodium. The reason for this is quite puzzling, since both alkalis have very similar physical and chemical properties (e.g. condensation and ionization proper- ties). Obtaining high-resolution transit observations of HD189733b and HD209458b, we were able to detect potassium on HD189733b (Manuscript 1), which was the first high-resolution detection of potassium on an exoplanet. The absence of potassium on HD209458b could be reasoned by depletion processes, such as condensation or photo-ionization or high-altitude clouds. In a further study (Manuscript II), we resolved the potassium line and compared this to a previously detected sodium absorption on this planet. The comparison showed, that the potassium lines are either tracing different altitudes and temperatures compared to the sodium lines, or are depleted so that the planetary Na/K- ratio is way larger than the stellar one. A comparison of the alkali lines with synthetic line profiles showed that the sodium lines were much broader than the potassium lines, probably being induced by winds. To investigate this, the effect of zonal streaming winds on the sodium lines on Jupiter-type planets is investigated in a further study (Manuscript III), showing that such winds can significantly broaden the Na- lines and that high-resolution observations can trace such winds with different properties. Furthermore, investigating the Na-line observations for different exoplanets, I showed that the Na-line broadening follows a trend with cooler planets showing stronger line broadening and so hinting on stronger winds, matching well into theoretical predictions. Each presented manuscript depends on the re- sults published within the previous manuscript, yielding a unitary study of the exoplanet HD189733b. The investigation of the potassium absorption required to account for different effects: The telluric lines removal and the effect of center-to-limb variation (see Manuscript I), the residual Rossiter-Mc-Laughlin effect (see Manuscript II) and the broadening of spectral lines on a translucent atmospheric ring by zonal jet streams (see Manuscript III). This thesis shows that high-resolution transmission spectroscopy is a powerful tool to probe sharp alkali line absorption on giant exoplanet atmospheres and to investigate on the properties and dynamics of hot Jupiter type atmospheres. KW - planets and satellites: atmospheres KW - planets and satellites: composition KW - planets and satellites: gaseous planets KW - exoplanets Y1 - 2021 ER - TY - JOUR A1 - Cherstvy, Andrey G. A1 - Thapa, Samudrajit A1 - Mardoukhi, Yousof A1 - Chechkin, Aleksei V. A1 - Metzler, Ralf T1 - Time averages and their statistical variation for the Ornstein-Uhlenbeck process BT - Role of initial particle distributions and relaxation to stationarity JF - Physical review : E, Statistical, nonlinear and soft matter physics N2 - How ergodic is diffusion under harmonic confinements? How strongly do ensemble- and time-averaged displacements differ for a thermally-agitated particle performing confined motion for different initial conditions? We here study these questions for the generic Ornstein-Uhlenbeck (OU) process and derive the analytical expressions for the second and fourth moment. These quantifiers are particularly relevant for the increasing number of single-particle tracking experiments using optical traps. For a fixed starting position, we discuss the definitions underlying the ensemble averages. We also quantify effects of equilibrium and nonequilibrium initial particle distributions onto the relaxation properties and emerging nonequivalence of the ensemble- and time-averaged displacements (even in the limit of long trajectories). We derive analytical expressions for the ergodicity breaking parameter quantifying the amplitude scatter of individual time-averaged trajectories, both for equilibrium and outof-equilibrium initial particle positions, in the entire range of lag times. Our analytical predictions are in excellent agreement with results of computer simulations of the Langevin equation in a parabolic potential. We also examine the validity of the Einstein relation for the ensemble- and time-averaged moments of the OU-particle. Some physical systems, in which the relaxation and nonergodic features we unveiled may be observable, are discussed. Y1 - 2018 U6 - https://doi.org/10.1103/PhysRevE.98.022134 SN - 2470-0045 SN - 2470-0053 VL - 98 IS - 2 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Schaerer, Daniel A1 - Izotov, Yuri I. A1 - Nakajima, K. A1 - Worseck, Gabor A1 - Chisholm, J. A1 - Verhamme, A. A1 - Thuan, T. X. A1 - de Barros, S. T1 - Intense C III] lambda lambda 1907,1909 emission from a strong Lyman continuum emitting galaxy JF - Astronomy and astrophysics : an international weekly journal N2 - We have obtained the first complete ultraviolet (UV) spectrum of a strong Lyman continuum (LyC) emitter at low redshift - the compact, low-metallicity, star-forming galaxy J1154+2443 - with a Lyman continuum escape fraction of 46% discovered recently. The Space Telescope Imaging Spectrograph spectrum shows strong Ly alpha and C III] lambda 1909 emission, as well as O III] lambda 1666. Our observations show that strong LyC emitters can have UV emission lines with a high equivalent width (e.g. EW(C III]) = 11.7 +/- 2.9 angstrom rest-frame), although their equivalent widths should be reduced due to the loss of ionizing photons. The intrinsic ionizing photon production efficiency of J1154+2443 is high, log(xi(0)(ion)) = 25.56 erg(-1) Hz, comparable to that of other recently discovered z similar to 0.3-0.4 LyC emitters. Combining our measurements and earlier determinations from the literature, we find a trend of increasing xi(0)(ion) with increasing C III] lambda 1909 equivalent width, which can be understood by a combination of decreasing stellar population age and metallicity. Simple ionization and density-bounded photoionization models can explain the main observational features including the UV spectrum of J1154+2443. KW - galaxies: starburst KW - galaxies: high-redshift KW - dark ages, reionization, first stars KW - ultraviolet: galaxies Y1 - 2018 U6 - https://doi.org/10.1051/0004-6361/201833823 SN - 1432-0746 VL - 616 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Battistoni, A. A1 - Dürr, H. A. A1 - Gühr, Markus A1 - Wolf, Thomas J. A. T1 - A tilted pulse-front setup for femtosecond transient grating spectroscopy in highly non-collinear geometries JF - Journal of optics N2 - We demonstrate a tilted pulse-front transient grating (TG) technique that allows to optimally utilize time resolution as well as TG line density while probing under grazing incidence as typically done in extreme ultraviolet (EUV) or soft x-ray (SXR) experiments. Our optical setup adapts the pulse front tilt of the two pulses that create the TG to the grazing incident pulse. We demonstrate the technique using all 800 nm femtosecond laser pulses for TG generation on a vanadium dioxide film. We probe that grating via diffraction of a third 800 nm pulse. The time resolution of 90 fs is an improvement by a factor of 30 compared to our previous experiments on the same system. The scheme paves the way for EUV and SXR probing of optically induced TGs on any material. KW - transient grating spectroscopy KW - ultrafast spectroscopy KW - pulse front matching Y1 - 2018 U6 - https://doi.org/10.1088/2040-8986/aad60a SN - 2040-8978 SN - 2040-8986 VL - 20 IS - 9 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Bustamante, Sebastian A1 - Sparre, Martin A1 - Springel, Volker A1 - Grand, Robert J. J. T1 - Merger-induced metallicity dilution in cosmological galaxy formation simulations JF - Monthly notices of the Royal Astronomical Society N2 - Observational studies have revealed that galaxy pairs tend to have lower gas-phase metallicity than isolated galaxies. This metallicity deficiency can be caused by inflows of low-metallicity gas due to the tidal forces and gravitational torques associated with galaxy mergers, diluting the metal content of the central region. In this work we demonstrate that such metallicity dilution occurs in state-of-the-art cosmological simulations of galaxy formation. We find that the dilution is typically 0.1 dex for major mergers, and is noticeable at projected separations smaller than 40 kpc. For minor mergers the metallicity dilution is still present, even though the amplitude is significantly smaller. Consistent with previous analysis of observed galaxies we find that mergers are outliers from the fundamental metallicity relation, with deviations being larger than expected for a Gaussian distribution of residuals. Our large sample of mergers within full cosmological simulations also makes it possible to estimate how the star formation rate enhancement and gas consumption timescale behave as a function of the merger mass ratio. We confirm that strong starbursts are likely to occur in major mergers, but they can also arise in minor mergers if more than two galaxies are participating in the interaction, a scenario that has largely been ignored in previous work based on idealised isolated merger simulations. KW - methods: numerical KW - galaxies: interactions KW - galaxies: star formation KW - galaxies: evolution Y1 - 2018 U6 - https://doi.org/10.1093/mnras/sty1692 SN - 0035-8711 SN - 1365-2966 VL - 479 IS - 3 SP - 3381 EP - 3392 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Cecchini, Gloria A1 - Thiel, Marco A1 - Schelter, Björn A1 - Sommerlade, Linda T1 - Improving network inference BT - the impact of false positive and false negative conclusions about the presence or absence of links JF - Journal of neuroscience methods N2 - Background: A reliable inference of networks from data is of key interest in the Neurosciences. Several methods have been suggested in the literature to reliably determine links in a network. To decide about the presence of links, these techniques rely on statistical inference, typically controlling the number of false positives, paying little attention to false negatives. New method: In this paper, by means of a comprehensive simulation study, we analyse the influence of false positive and false negative conclusions about the presence or absence of links in a network on the network topology. We show that different values to balance false positive and false negative conclusions about links should be used in order to reliably estimate network characteristics. We propose to run careful simulation studies prior to making potentially erroneous conclusion about the network topology. Results: Our analysis shows that optimal values to balance false positive and false negative conclusions about links depend on the network topology and characteristic of interest. Comparison with existing methods: Existing methods rely on a choice of the rate for false positive conclusions. They aim to be sure about individual links rather than the entire network. The rate of false negative conclusions is typically not investigated. Conclusions: Our investigation shows that the balance of false positive and false negative conclusions about links in a network has to be tuned for any network topology that is to be estimated. Moreover, within the same network topology, the results are qualitatively the same for each network characteristic, but the actual values leading to reliable estimates of the characteristics are different. KW - Network inference KW - Node degree distribution KW - False positive KW - False negative KW - Statistical inference Y1 - 2018 U6 - https://doi.org/10.1016/j.jneumeth.2018.06.011 SN - 0165-0270 SN - 1872-678X VL - 307 SP - 31 EP - 36 PB - Elsevier CY - Amsterdam ER - TY - JOUR A1 - Heintz, Kasper Elm A1 - Watson, D. A1 - Jakobsson, P. A1 - Fynbo, J. P. U. A1 - Bolmer, J. A1 - Arabsalmani, M. A1 - Cano, Zach A1 - Covino, S. A1 - Gomboc, A. A1 - Japelj, J. A1 - Kaper, L. A1 - Krogager, J. -K. A1 - Pugliese, G. A1 - Sanchez-Ramirez, R. A1 - Selsing, J. A1 - Sparre, Martin A1 - Tanvir, N. R. A1 - Thone, C. C. A1 - de Ugarte Postigo, A. A1 - Vergani, S. D. T1 - Highly ionized metals as probes of the circumburst gas in the natal regions of gamma-ray bursts JF - Monthly notices of the Royal Astronomical Society N2 - We present here a survey of high-ionization absorption lines in the afterglow spectra of long-duration gamma-ray bursts (GRBs) obtained with the VLT/X-shooter spectrograph. Our main goal is to investigate the circumburst medium in the natal regions of GRBs. Our primary focus is on the N vλλ 1238, 1242 line transitions, but we also discuss other high-ionization lines such as O vi, C iv, and Si iv. We find no correlation between the column density of N v and the neutral gas properties such as metallicity, H i column density, and dust depletion; however, the relative velocity of N v, typically a blueshift with respect to the neutral gas, is found to be correlated with the column density of H i. This may be explained if the N v gas is part of an H ii region hosting the GRB, where the region’s expansion is confined by dense, neutral gas in the GRB’s host galaxy. We find tentative evidence (at 2σ significance) that the X-ray derived column density, NH, X, may be correlated with the column density of N v, which would indicate that both measurements are sensitive to the column density of the gas located in the vicinity of the GRB. We investigate the scenario where N v (and also O vi) is produced by recombination after the corresponding atoms have been stripped entirely of their electrons by the initial prompt emission, in contrast to previous models where highly ionized gas is produced by photoionization from the GRB afterglow. KW - gamma-ray bursts: general KW - ISM: abundances Y1 - 2018 U6 - https://doi.org/10.1093/mnras/sty1447 SN - 0035-8711 SN - 1365-2966 VL - 479 IS - 3 SP - 3456 EP - 3476 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Lebiga, O. A1 - Santos-Lima, Reinaldo A1 - Yan, Huirong T1 - Kinetic-MHD simulations of gyroresonance instability driven by CR pressure anisotropy JF - Monthly notices of the Royal Astronomical Society N2 - The transport of cosmic rays (CRs) is crucial for the understanding of almost all high-energy phenomena. Both pre-existing large-scale magnetohydrodynamic (MHD) turbulence and locally generated turbulence through plasma instabilities are important for the CR propagation in astrophysical media. The potential role of the resonant instability triggered by CR pressure anisotropy to regulate the parallel spatial diffusion of low-energy CRs (less than or similar to 100 GeV) in the interstellar and intracluster medium of galaxies has been shown in previous theoretical works. This work aims to study the gyroresonance instability via direct numerical simulations, in order to access quantitatively the wave-particle scattering rates. For this, we employ a 1D PIC-MHD code to follow the growth and saturation of the gyroresonance instability. We extract from the simulations the pitch-angle diffusion coefficient D-mu mu produced by the instability during the linear and saturation phases, and a very good agreement (within a factor of 3) is found with the values predicted by the quasi-linear theory (QLT). Our results support the applicability of the QLT for modelling the scattering of low-energy CRs by the gyroresonance instability in the complex interplay between this instability and the large-scale MHD turbulence. KW - MHD KW - plasmas KW - turbulence KW - cosmic rays Y1 - 2018 U6 - https://doi.org/10.1093/mnras/sty309 SN - 0035-8711 SN - 1365-2966 VL - 476 IS - 2 SP - 2779 EP - 2791 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - El-Nagar, Gumaa A. A1 - Lauermann, Iver A1 - Sarhan, Radwan Mohamed A1 - Roth, Christina T1 - Hierarchically structured iron-doped silver (Ag-Fe) lotus flowers for an efficient oxygen reduction reaction JF - Nanoscale N2 - The development of cheap and efficient electrocatalysts for the oxygen reduction reaction (ORR) is vital for the immediate commercialization of fuel cells which are still limited by the high cost and low performance of the utilized commercial Pt-based electrodes. As a promising alternative, this study reports on the synthesis of hierarchical iron-doped silver lotus flowers (AgFelotus) by a facile chemical procedure as robust and efficient ORR electrocatalysts. Succinic acid was used as a structure directing agent to tune the morphology of undoped and iron-doped silver particles. In the absence of succinic acid, ball-like silver particles were obtained, while using 2 mM succinic acid led to peony-like flower structures. The doping of silver peony-flowers with iron resulted in lotus-like flower structures with high electrocatalytic activity for ORR together with outstanding tolerance against poisoning with various hydrocarbon (HC) impurities, in situ generated during fuel cell operation, as well as different fuels from anodic crossover. AgFelotus exhibited a superior ORR activity with more than 40 times higher stability than the commercial Pt/C catalyst in alkaline media. This substantial performance enhancement is attributed to the unique lotus-like flower structures providing more electroactive surface sites, in addition to the iron dopants which facilitate ORR charge transfer. Y1 - 2018 U6 - https://doi.org/10.1039/c8nr00020d SN - 2040-3364 SN - 2040-3372 VL - 10 IS - 15 SP - 7304 EP - 7310 PB - Royal Society of Chemistry CY - Cambridge ER - TY - JOUR A1 - Zhang, Heshou A1 - Yan, Huirong A1 - Richter, Philipp T1 - The influence of atomic alignment on absorption and emission spectroscopy JF - Monthly notices of the Royal Astronomical Society N2 - Spectroscopic observations play essential roles in astrophysics. They are crucial for determining physical parameters in our Universe, providing information about the chemistry of various astronomical environments. The proper execution of the spectroscopic analysis requires accounting for all the physical effects that are compatible to the signal-to-noise ratio. We find in this paper the influence on spectroscopy from the atomic/ground state alignment owing to anisotropic radiation and modulated by interstellar magnetic field, has significant impact on the study of interstellar gas. In different observational scenarios, we comprehensively demonstrate how atomic alignment influences the spectral analysis and provide the expressions for correcting the effect. The variations are even more pronounced for multiplets and line ratios. We show the variation of the deduced physical parameters caused by the atomic alignment effect, including alpha-to-iron ratio ([X/Fe]) and ionization fraction. Synthetic observations are performed to illustrate the visibility of such effect with current facilities. A study of Photodissociation regions in rho Ophiuchi cloud is presented to demonstrate how to account for atomic alignment in practice. Our work has shown that due to its potential impact, atomic alignment has to be included in an accurate spectroscopic analysis of the interstellar gas with current observational capability. KW - magnetic fields KW - submillimetre: ISM KW - ultraviolet: ISM KW - ISM: abundances KW - ISM: lines and bands KW - techniques: spectroscopic Y1 - 2018 U6 - https://doi.org/10.1093/mnras/sty1594 SN - 0035-8711 SN - 1365-2966 VL - 479 IS - 3 SP - 3923 EP - 3935 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Schmidt, Tobias M. A1 - Hennawi, Joseph F. A1 - Worseck, Gabor A1 - Davies, Frederick B. A1 - Lukic, Zarija A1 - Oñorbe, Jose T1 - Modeling the HeII transverse proximity effect BT - constraints on quasar lifetime and obscuration JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - The He II transverse proximity effect-enhanced He II Ly alpha transmission in a background sightline caused by the ionizing radiation of a foreground quasar-offers a unique opportunity to probe the emission properties of quasars, in particular the emission geometry (obscuration, beaming) and the quasar lifetime. Building on the foreground quasar survey published in Schmidt et al., we present a detailed model of the He II transverse proximity effect, specifically designed to include light travel time effects, finite quasar ages, and quasar obscuration. We postprocess outputs from a cosmological hydrodynamical simulation with a fluctuating He II ultraviolet background model, with the added effect of the radiation from a single bright foreground quasar. We vary the age t(age) and obscured sky fractions Omega(obsc) of the foreground quasar, and explore the resulting effect on the He II transverse proximity effect signal. Fluctuations in intergalactic medium density and the ultraviolet background, as well as the unknown orientation of the foreground quasar, result in a large variance of the He II Ly alpha transmission along the background sightline. We develop a fully Bayesian statistical formalism to compare far-ultraviolet He II Ly alpha transmission spectra of the background quasars to our models, and extract joint constraints on t(age) and Omega(obsc) for the six Schmidt et al. foreground quasars with the highest implied He II photoionization rates. Our analysis suggests a bimodal distribution of quasar emission properties, whereby one foreground quasar, associated with a strong He II transmission spike, is relatively old (22 Myr) and unobscured (Omega(obsc) < 35%), whereas three others are either younger than 10 Myr or highly obscured (Omega(obsc) > 70%). KW - dark ages, reionization, first stars KW - intergalactic medium KW - quasars: general Y1 - 2018 U6 - https://doi.org/10.3847/1538-4357/aac8e4 SN - 0004-637X SN - 1538-4357 VL - 861 IS - 2 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Yang, Jie A1 - Zhu, Xiaolei A1 - Wolf, Thomas J. A. A1 - Li, Zheng A1 - Nunes, João Pedro Figueira A1 - Coffee, Ryan A1 - Cryan, James P. A1 - Gühr, Markus A1 - Hegazy, Kareem A1 - Heinz, Tony F. A1 - Jobe, Keith A1 - Li, Renkai A1 - Shen, Xiaozhe A1 - Veccione, Theodore A1 - Weathersby, Stephen A1 - Wilkin, Kyle J. A1 - Yoneda, Charles A1 - Zheng, Qiang A1 - Martinez, Todd J. A1 - Centurion, Martin A1 - Wang, Xijie T1 - Imaging CF3I conical intersection and photodissociation dynamics with ultrafast electron diffraction JF - Science N2 - Conical intersections play a critical role in excited-state dynamics of polyatomic molecules because they govern the reaction pathways of many nonadiabatic processes. However, ultrafast probes have lacked sufficient spatial resolution to image wave-packet trajectories through these intersections directly. Here, we present the simultaneous experimental characterization of one-photon and two-photon excitation channels in isolated CF3I molecules using ultrafast gas-phase electron diffraction. In the two-photon channel, we have mapped out the real-space trajectories of a coherent nuclear wave packet, which bifurcates onto two potential energy surfaces when passing through a conical intersection. In the one-photon channel, we have resolved excitation of both the umbrella and the breathing vibrational modes in the CF3 fragment in multiple nuclear dimensions. These findings benchmark and validate ab initio nonadiabatic dynamics calculations. Y1 - 2018 U6 - https://doi.org/10.1126/science.aat0049 SN - 0036-8075 SN - 1095-9203 VL - 361 IS - 6397 SP - 64 EP - 67 PB - American Assoc. for the Advancement of Science CY - Washington ER - TY - JOUR A1 - Ohm, Stefan A1 - Hoischen, Clemens T1 - On the expected gamma-ray emission from nearby flaring stars JF - Monthly notices of the Royal Astronomical Society N2 - Stellar flares have been extensively studied in soft X-rays (SXRs) by basically every X-ray mission. Hard X-ray (HXR) emission from stellar superflares, however, have only been detected from a handful of objects over the past years. One very extreme event was the superflare from the young M-dwarf DGCVn binary star system, which triggered Swift/BAT as if it was a gamma-ray burst. In this work, we estimate the expected gamma-ray emission from DGCVn and the most extreme stellar flares by extrapolating from solar flares based on measured solar energetic particles (SEPs), as well as thermal and non-thermal emission properties. We find that ions are plausibly accelerated in stellar superflares to 100 GeV energies, and possibly up to TeV energies in the associated coronal mass ejections. The corresponding pi(0)-decay gamma-ray emission could be detectable from stellar superflares with ground-based gamma-ray telescopes. On the other hand, the detection of gamma-ray emission implies particle densities high enough that ions suffer significant losses due to inelastic proton-proton scattering. The next-generation Cherenkov Telescope Array (CTA) should be able to probe superflares from M dwarfs in the solar neighbourhood and constrain the energy in interacting cosmic rays and/or their maximum energy. The detection of gamma-ray emission from stellar flares would open a new window for the study of stellar physics, the underlying physical processes in flares and their impact on habitability of planetary systems. KW - radiation mechanisms: non-thermal KW - stars: flare KW - stars: individual: DGCVn-gamma rays: stars Y1 - 2018 U6 - https://doi.org/10.1093/mnras/stx2806 SN - 0035-8711 SN - 1365-2966 VL - 474 IS - 1 SP - 1335 EP - 1341 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Benini, Marco A1 - Schenkel, Alexander A1 - Schreiber, Urs T1 - The Stack of Yang-Mills Fields on Lorentzian Manifolds JF - Communications in mathematical physics N2 - We provide an abstract definition and an explicit construction of the stack of non-Abelian Yang-Mills fields on globally hyperbolic Lorentzian manifolds. We also formulate a stacky version of the Yang-Mills Cauchy problem and show that its well-posedness is equivalent to a whole family of parametrized PDE problems. Our work is based on the homotopy theoretical approach to stacks proposed in Hollander (Isr. J. Math. 163:93-124, 2008), which we shall extend by further constructions that are relevant for our purposes. In particular, we will clarify the concretification of mapping stacks to classifying stacks such as BG (con). Y1 - 2018 U6 - https://doi.org/10.1007/s00220-018-3120-1 SN - 0010-3616 SN - 1432-0916 VL - 359 IS - 2 SP - 765 EP - 820 PB - Springer CY - New York ER - TY - JOUR A1 - Koopman, Wouter-Willem Adriaan A1 - Muccini, Michele A1 - Toffanin, Stefano T1 - High-resolution photoluminescence electro-modulation microscopy by scanning lock-in JF - Review of scientific instruments : a monthly journal devoted to scientific instruments, apparatus, and techniques N2 - Morphological inhomogeneities and structural defects in organic semiconductors crucially determine the charge accumulation and lateral transport in organic thin-film transistors. Photoluminescence Electro-Modulation (PLEM) microscopy is a laser-scanning microscopy technique that relies on the modulation of the thin-film fluorescence in the presence of charge-carriers to image the spatial distribution of charges within the active organic semiconductor. Here, we present a lock-in scheme based on a scanning beam approach for increasing the PLEM microscopy resolution and contrast. The charge density in the device is modulated by a sinusoidal electrical signal, phase-locked to the scanning beam of the excitation laser. The lock-in detection scheme is achieved by acquiring a series of images with different phases between the beam scan and the electrical modulation. Application of high resolution PLEM to an organic transistor in accumulation mode demonstrates its potential to image local variations in the charge accumulation. A diffraction-limited precision of sub-300 nm and a signal to noise ratio of 21.4 dB could be achieved. Published by AIP Publishing. Y1 - 2018 U6 - https://doi.org/10.1063/1.5010281 SN - 0034-6748 SN - 1089-7623 VL - 89 IS - 4 PB - American Institute of Physics CY - Melville ER - TY - JOUR A1 - Mor, Selene A1 - Herzog, Marc A1 - Noack, Johannes A1 - Katayama, Naoyuki A1 - Nohara, Minoru A1 - Takagi, Hide A1 - Trunschke, Annette A1 - Mizokawa, Takashi A1 - Monney, Claude A1 - Stähler, Julia T1 - Inhibition of the photoinduced structural phase transition in the excitonic insulator Ta2NiSe5 JF - Physical review : B, Condensed matter and materials physics N2 - Femtosecond time-resolved midinfrared reflectivity is used to investigate the electron and phonon dynamics occurring at the direct band gap of the excitonic insulator Ta2NiSe5 below the critical temperature of its structural phase transition. We find that the phonon dynamics show a strong coupling to the excitation of free carriers at the Gamma point of the Brillouin zone. The optical response saturates at a critical excitation fluence F-C = 0.30 +/- 0.08 mJ/cm(2) due to optical absorption saturation. This limits the optical excitation density in Ta2NiSe5 so that the system cannot be pumped sufficiently strongly to undergo the structural change to the high-temperature phase. We thereby demonstrate that Ta2NiSe5 exhibits a blocking mechanism when pumped in the near-infrared regime, preventing a nonthermal structural phase transition. Y1 - 2018 U6 - https://doi.org/10.1103/PhysRevB.97.115154 SN - 2469-9950 SN - 2469-9969 VL - 97 IS - 11 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Aydiner, Ekrem A1 - Cherstvy, Andrey G. A1 - Metzler, Ralf T1 - Wealth distribution, Pareto law, and stretched exponential decay of money BT - Computer simulations analysis of agent-based models JF - Physica : europhysics journal ; A, Statistical mechanics and its applications N2 - We study by Monte Carlo simulations a kinetic exchange trading model for both fixed and distributed saving propensities of the agents and rationalize the person and wealth distributions. We show that the newly introduced wealth distribution – that may be more amenable in certain situations – features a different power-law exponent, particularly for distributed saving propensities of the agents. For open agent-based systems, we analyze the person and wealth distributions and find that the presence of trap agents alters their amplitude, leaving however the scaling exponents nearly unaffected. For an open system, we show that the total wealth – for different trap agent densities and saving propensities of the agents – decreases in time according to the classical Kohlrausch–Williams–Watts stretched exponential law. Interestingly, this decay does not depend on the trap agent density, but rather on saving propensities. The system relaxation for fixed and distributed saving schemes are found to be different. KW - Econophysics KW - Wealth and income distribution KW - Pareto law KW - Scaling exponents Y1 - 2017 U6 - https://doi.org/10.1016/j.physa.2017.08.017 SN - 0378-4371 SN - 1873-2119 VL - 490 SP - 278 EP - 288 PB - Elsevier CY - Amsterdam ER - TY - JOUR A1 - Totz, Sonja Juliana A1 - Eliseev, Alexey V. A1 - Petri, Stefan A1 - Flechsig, Michael A1 - Caesar, Levke A1 - Petoukhov, Vladimir A1 - Coumou, Dim T1 - The dynamical core of the Aeolus 1.0 statistical-dynamical atmosphere model BT - validation and parameter optimization JF - Geoscientific model development : an interactive open access journal of the European Geosciences Union N2 - Here, we present novel equations for the large-scale zonal-mean wind as well as those for planetary waves. Together with synoptic parameterization (as presented by Coumou et al., 2011), these form the mathematical description of the dynamical core of Aeolus 1.0. The regions of high azonal wind velocities (planetary waves) are accurately captured for all validation experiments. The zonal-mean zonal wind and the integrated lower troposphere mass flux show good results in particular in the Northern Hemisphere. In the Southern Hemisphere, the model tends to produce too-weak zonal-mean zonal winds and a too-narrow Hadley circulation. We discuss possible reasons for these model biases as well as planned future model improvements and applications. Y1 - 2018 U6 - https://doi.org/10.5194/gmd-11-665-2018 SN - 1991-959X SN - 1991-9603 VL - 11 IS - 2 SP - 665 EP - 679 PB - Copernicus CY - Göttingen ER - TY - JOUR A1 - Xiong, Hui A1 - Fang, Li A1 - Osipov, Timur A1 - Kling, Nora G. A1 - Wolf, Thomas J. A. A1 - Sistrunk, Emily A1 - Obaid, Razib A1 - Gühr, Markus A1 - Berrah, Nora T1 - Fragmentation of endohedral fullerene Ho3N@C-80 in an intense femtosecond near-infrared laser field JF - Physical review : A, Atomic, molecular, and optical physics N2 - The fragmentation of gas phase endohedral fullerene, Ho3N@C-80, was investigated using femtosecond near-infrared laser pulses with an ion velocity map imaging spectrometer. We observed that Ho+ abundance associated with carbon cage opening dominates at an intensity of 1.1 x 10(14) W/cm(2). As the intensity increases, the Ho+ yield associated with multifragmentation of the carbon cage exceeds the prominence of Ho+ associated with the gentler carbon cage opening. Moreover, the power law dependence of Ho+ on laser intensity indicates that the transition of the most likely fragmentation mechanisms occurs around 2.0 x 10(14) W/cm(2). Y1 - 2018 U6 - https://doi.org/10.1103/PhysRevA.97.023419 SN - 2469-9926 SN - 2469-9934 VL - 97 IS - 2 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Fox, Andrew J. A1 - Barger, Kathleen A. A1 - Wakker, Bart P. A1 - Richter, Philipp A1 - Antwi-Danso, Jacqueline A1 - Casetti-Dinescu, Dana I. A1 - Howk, J. Christopher A1 - Lehner, Nicolas A1 - Crowther, Paul A. A1 - Lockman, Felix J. T1 - Chemical Abundances in the Leading Arm of the Magellanic Stream JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - The Leading Arm (LA) of the Magellanic Stream is a vast debris field of H I clouds connecting the Milky Way and the Magellanic Clouds. It represents an example of active gas accretion onto the Galaxy. Previously, only one chemical abundance measurement had been made in the LA. Here we present chemical abundance measurements using Hubble Space Telescope/Cosmic Origins Spectrograph and Green Bank Telescope spectra of four AGN sightlines passing through the LA and three nearby sightlines that may trace outer fragments of the LA. We find low oxygen abundances, ranging from 4.0+(2.0)(2.0)% 12.6(4.1)(6.0)% solar, in the confirmed LA directions, with the lowest values found in the region known as LA III, farthest from the LMC. These abundances are substantially lower than the single previous measurement, S/H = 35 +/- 7% solar, but are in agreement with those reported in the SMC filament of the trailing Stream, supporting a common origin in the SMC (not the LMC) for the majority of the LA and trailing Stream. This provides important constraints for models of the formation of the Magellanic System. Finally, two of the three nearby sightlines show high-velocity clouds with H I columns, kinematics, and oxygen abundances consistent with LA membership. This suggests that the LA is larger than traditionally thought, extending at least 20 degrees further to the Galactic northwest. KW - Galaxy: evolution KW - Galaxy: halo KW - ISM: abundances KW - Magellanic Clouds KW - quasars: absorption lines Y1 - 2018 U6 - https://doi.org/10.3847/1538-4357/aaa9bb SN - 0004-637X SN - 1538-4357 VL - 854 IS - 2 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Young, Linda A1 - Ueda, Kiyoshi A1 - Gühr, Markus A1 - Bucksbaum, Philip H. A1 - Simon, Marc A1 - Mukamel, Shaul A1 - Rohringer, Nina A1 - Prince, Kevin C. A1 - Masciovecchio, Claudio A1 - Meyer, Michael A1 - Rudenko, Artem A1 - Rolles, Daniel A1 - Bostedt, Christoph A1 - Fuchs, Matthias A1 - Reis, David A. A1 - Santra, Robin A1 - Kapteyn, Henry A1 - Murnane, Margaret A1 - Ibrahim, Heide A1 - Legare, Francois A1 - Vrakking, Marc A1 - Isinger, Marcus A1 - Kroon, David A1 - Gisselbrecht, Mathieu A1 - Wörner, Hans Jakob A1 - Leone, Stephen R. T1 - Roadmap of ultrafast x-ray atomic and molecular physics JF - Journal of physics : B, Atomic, molecular and optical physics N2 - X-ray free-electron lasers (XFELs) and table-top sources of x-rays based upon high harmonic generation (HHG) have revolutionized the field of ultrafast x-ray atomic and molecular physics, largely due to an explosive growth in capabilities in the past decade. XFELs now provide unprecedented intensity (10(20) W cm(-2)) of x-rays at wavelengths down to similar to 1 Angstrom, and HHG provides unprecedented time resolution (similar to 50 attoseconds) and a correspondingly large coherent bandwidth at longer wavelengths. For context, timescales can be referenced to the Bohr orbital period in hydrogen atom of 150 attoseconds and the hydrogen-molecule vibrational period of 8 femtoseconds; wavelength scales can be referenced to the chemically significant carbon K-edge at a photon energy of similar to 280 eV (44 Angstroms) and the bond length in methane of similar to 1 Angstrom. With these modern x-ray sources one now has the ability to focus on individual atoms, even when embedded in a complex molecule, and view electronic and nuclear motion on their intrinsic scales (attoseconds and Angstroms). These sources have enabled coherent diffractive imaging, where one can image non-crystalline objects in three dimensions on ultrafast timescales, potentially with atomic resolution. The unprecedented intensity available with XFELs has opened new fields of multiphoton and nonlinear x-ray physics where behavior of matter under extreme conditions can be explored. The unprecedented time resolution and pulse synchronization provided by HHG sources has kindled fundamental investigations of time delays in photoionization, charge migration in molecules, and dynamics near conical intersections that are foundational to AMO physics and chemistry. This roadmap coincides with the year when three new XFEL facilities, operating at Angstrom wavelengths, opened for users (European XFEL, Swiss-FEL and PAL-FEL in Korea) almost doubling the present worldwide number of XFELs, and documents the remarkable progress in HHG capabilities since its discovery roughly 30 years ago, showcasing experiments in AMO physics and other applications. Here we capture the perspectives of 17 leading groups and organize the contributions into four categories: ultrafast molecular dynamics, multidimensional x-ray spectroscopies; high-intensity x-ray phenomena; attosecond x-ray science. KW - ultrafast molecular dynamics KW - x-ray spectroscopies and phenomena KW - table-top sources KW - x-ray free-electron lasers KW - attosecond phenomena Y1 - 2018 U6 - https://doi.org/10.1088/1361-6455/aa9735 SN - 0953-4075 SN - 1361-6455 VL - 51 IS - 3 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Myhre, Rolf H. A1 - Wolf, Thomas J. A. A1 - Cheng, Lan A1 - Nandi, Saikat A1 - Coriani, Sonia A1 - Gühr, Markus A1 - Koch, Henrik T1 - A theoretical and experimental benchmark study of core-excited states in nitrogen JF - The journal of chemical physics : bridges a gap between journals of physics and journals of chemistr N2 - The high resolution near edge X-ray absorption fine structure spectrum of nitrogen displays the vibrational structure of the core-excited states. This makes nitrogen well suited for assessing the accuracy of different electronic structure methods for core excitations. We report high resolution experimental measurements performed at the SOLEIL synchrotron facility. These are compared with theoretical spectra calculated using coupled cluster theory and algebraic diagrammatic construction theory. The coupled cluster singles and doubles with perturbative triples model known as CC3 is shown to accurately reproduce the experimental excitation energies as well as the spacing of the vibrational transitions. The computational results are also shown to be systematically improved within the coupled cluster hierarchy, with the coupled cluster singles, doubles, triples, and quadruples method faithfully reproducing the experimental vibrational structure. Published by AIP Publishing. Y1 - 2018 U6 - https://doi.org/10.1063/1.5011148 SN - 0021-9606 SN - 1089-7690 VL - 148 IS - 6 PB - American Institute of Physics CY - Melville ER - TY - JOUR A1 - Zellmeier, M. A1 - Brenner, Thomas J. K. A1 - Janietz, Silvia A1 - Nickel, N. H. A1 - Rappich, J. T1 - Polythiophenes as emitter layers for crystalline silicon solar cells BT - parasitic absorption, interface passivation, and open circuit voltage JF - Journal of applied physics N2 - We investigated the influence of the emitter (amorphous-Si, a-Si, or polythiophene derivatives: poly(3-hexylthiophene), P3HT, and poly(3-[3,6-dioxaheptyl]-thiophene), P3DOT) and the interface passivation (intrinsic a-Si or SiOX and methyl groups or SiOX) on the c-Si based 1 × 1 cm2 planar hybrid heterojunction solar cell parameters. We observed higher short circuit currents for the P3HT or P3DOT/c-Si solar cells than those obtained for a-Si/c-Si devices, independent of the interface passivation. The obtained VOC of 659 mV for the P3DOT/SiOX/c-Si heterojunction solar cell with hydrophilic 3,6-dioxaheptyl side chains is among the highest reported for c-Si/polythiophene devices. The maximum power conversion efficiency, PCE, was 11% for the P3DOT/SiOX/c-Si heterojunction solar cell. Additionally, our wafer lifetime measurements reveal a field effect passivation in the wafer induced by the polythiophenes when deposited on c-Si. Y1 - 2018 U6 - https://doi.org/10.1063/1.5006625 SN - 0021-8979 SN - 1089-7550 VL - 123 IS - 3 PB - American Institute of Physics CY - Melville ER - TY - JOUR A1 - Sawicki, Jakub A1 - Abel, Markus A1 - Schöll, Eckehard T1 - Synchronization of organ pipes JF - The European physical journal : B, Condensed matter and complex systems N2 - We investigate synchronization of coupled organ pipes. Synchronization and reflection in the organ lead to undesired weakening of the sound in special cases. Recent experiments have shown that sound interaction is highly complex and nonlinear, however, we show that two delay-coupled Van-der-Pol oscillators appear to be a good model for the occurring dynamical phenomena. Here the coupling is realized as distance-dependent, or time-delayed, equivalently. Analytically, we investigate the synchronization frequency and bifurcation scenarios which occur at the boundaries of the Arnold tongues. We successfully compare our results to experimental data. Y1 - 2018 U6 - https://doi.org/10.1140/epjb/e2017-80485-8 SN - 1434-6028 SN - 1434-6036 VL - 91 IS - 2 PB - Springer CY - New York ER - TY - GEN A1 - Javanainen, Matti A1 - Martinez-Seara, Hector A1 - Metzler, Ralf A1 - Vattulainen, Ilpo Tapio T1 - Diffusion of Proteins and Lipids in Protein-Rich Membranesa T2 - Biophysical journal Y1 - 2018 U6 - https://doi.org/10.1016/j.bpj.2017.11.3009 SN - 0006-3495 SN - 1542-0086 VL - 114 IS - 3 SP - 551A EP - 551A PB - Cell Press CY - Cambridge ER - TY - JOUR A1 - Krapf, Diego A1 - Marinari, Enzo A1 - Metzler, Ralf A1 - Oshanin, Gleb A1 - Xu, Xinran A1 - Squarcini, Alessio T1 - Power spectral density of a single Brownian trajectory BT - what one can and cannot learn from it JF - New journal of physics : the open-access journal for physics N2 - The power spectral density (PSD) of any time-dependent stochastic processX (t) is ameaningful feature of its spectral content. In its text-book definition, the PSD is the Fourier transform of the covariance function of X-t over an infinitely large observation timeT, that is, it is defined as an ensemble-averaged property taken in the limitT -> infinity. Alegitimate question is what information on the PSD can be reliably obtained from single-trajectory experiments, if one goes beyond the standard definition and analyzes the PSD of a single trajectory recorded for a finite observation timeT. In quest for this answer, for a d-dimensional Brownian motion (BM) we calculate the probability density function of a single-trajectory PSD for arbitrary frequency f, finite observation time T and arbitrary number k of projections of the trajectory on different axes. We show analytically that the scaling exponent for the frequency-dependence of the PSD specific to an ensemble of BM trajectories can be already obtained from a single trajectory, while the numerical amplitude in the relation between the ensemble-averaged and single-trajectory PSDs is afluctuating property which varies from realization to realization. The distribution of this amplitude is calculated exactly and is discussed in detail. Our results are confirmed by numerical simulations and single-particle tracking experiments, with remarkably good agreement. In addition we consider a truncated Wiener representation of BM, and the case of a discrete-time lattice random walk. We highlight some differences in the behavior of a single-trajectory PSD for BM and for the two latter situations. The framework developed herein will allow for meaningful physical analysis of experimental stochastic trajectories. KW - power spectral density KW - single-trajectory analysis KW - probability density function KW - exact results Y1 - 2018 U6 - https://doi.org/10.1088/1367-2630/aaa67c SN - 1367-2630 VL - 20 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Leiendecker, Mai-Thi A1 - Licht, Christopher J. A1 - Borghs, Jannik A1 - Mooney, David J. A1 - Zimmermann, Marc A1 - Böker, Alexander T1 - Physical polyurethane hydrogels via charge shielding through acids or salts JF - Macromolecular rapid communications N2 - Physical hydrogels with tunable stress-relaxation and excellent stress recovery are formed from anionic polyurethanes via addition of acids, monovalent salts, or divalent salts. Gel properties can be widely adjusted through pH, salt valence, salt concentration, and monomer composition. We propose and investigate a novel gelation mechanism based on a colloidal system interacting through charge repulsion and chrage shielding, allowing a broad use of the material, from acidic (pH 4–5.5) to pH-neutral hydrogels with Young's moduli ranging from 10 to 140 kPa. KW - acidic crosslinking KW - charge repulsion KW - charge shielding KW - ionic crosslinking KW - physical hydrogels KW - polyurethanes KW - stress recovery KW - stress-relaxation Y1 - 2018 U6 - https://doi.org/10.1002/marc.201700711 SN - 1022-1336 SN - 1521-3927 VL - 39 IS - 7 PB - Wiley-VCH CY - Weinheim ER - TY - JOUR A1 - Sachse, Manuel T1 - A planetary dust ring generated by impact-ejection from the Galilean satellites JF - Icarus : international journal of solar system studies N2 - All outer planets in the Solar System are surrounded by a ring system. Many of these rings are dust rings or they contain at least a high proportion of dust. They are often formed by impacts of micro-meteoroids onto embedded bodies. The ejected material typically consists of micron-sized charged particles, which are susceptible to gravitational and non-gravitational forces. Generally, detailed information on the dynamics and distribution of the dust requires expensive numerical simulations of a large number of particles. Here we develop a relatively simple and fast, semi-analytical model for an impact-generated planetary dust ring governed by the planet’s gravity and the relevant perturbation forces for the dynamics of small charged particles. The most important parameter of the model is the dust production rate, which is a linear factor in the calculation of the dust densities. We apply our model to dust ejected from the Galilean satellites using production rates obtained from flybys of the dust sources. The dust densities predicted by our model are in good agreement with numerical simulations and with in situ measurements by the Galileo spacecraft. The lifetimes of large particles are about two orders of magnitude greater than those of small ones, which implies a flattening of the size distribution in circumplanetary space. Information about the distribution of circumplanetary dust is also important for the risk assessment of spacecraft orbits in the respective regions. Y1 - 0207 U6 - https://doi.org/10.1016/j.icarus.2017.10.011 SN - 0019-1035 SN - 1090-2643 VL - 303 SP - 166 EP - 180 PB - Elsevier CY - San Diego ER - TY - GEN A1 - Gudowska-Nowak, Ewa A1 - Lindenberg, Katja A1 - Metzler, Ralf T1 - Preface: Marian Smoluchowski’s 1916 paper—a century of inspiration T2 - Journal of physics : A, Mathematical and theoretical Y1 - 2017 U6 - https://doi.org/10.1088/1751-8121/aa8529 SN - 1751-8113 SN - 1751-8121 VL - 50 IS - 38 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Cheng, Xin A1 - Kliem, Bernhard A1 - Ding, Mingde T1 - Unambiguous evidence of filament splitting-induced partial eruptions JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - Coronal mass ejections are often considered to result from the full eruption of a magnetic flux rope (MFR). However, it is recognized that, in some events, the MFR may release only part of its flux, with the details of the implied splitting not completely established due to limitations in observations. Here, we investigate two partial eruption events including a confined and a successful one. Both partial eruptions are a consequence of the vertical splitting of a filament-hosting MFR involving internal reconnection. A loss of equilibrium in the rising part of the magnetic flux is suggested by the impulsive onset of both events and by the delayed onset of reconnection in the confined event. The remaining part of the flux might be line-tied to the photosphere in a bald patch (BP) separatrix surface, and we confirm the existence of extended BP sections for the successful eruption. The internal reconnection is signified by brightenings in the body of one filament and between the rising and remaining parts of both filaments. It evolves quickly into the standard current sheet reconnection in the wake of the eruption. As a result, regardless of being confined or successful, both eruptions produce hard X-ray sources and flare loops below the erupting but above the surviving flux, as well as a pair of flare ribbons enclosing the latter. KW - Sun: magnetic fields KW - Sun: corona KW - Sun: coronal mass ejections (CMEs) KW - Sun: flares Y1 - 2018 U6 - https://doi.org/10.3847/1538-4357/aab08d SN - 0004-637X SN - 1538-4357 VL - 856 IS - 1 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Baushev, Anton N. A1 - Barkov, M. V. T1 - Why does Einasto profile index n similar to 6 occur so frequently? JF - Journal of cosmology and astroparticle physics N2 - We consider the behavior of spherically symmetric Einasto halos composed of gravitating particles in the Fokker-Planck approximation. This approach allows us to consider the undesirable influence of close encounters in the N-body simulations more adequately than the generally accepted criteria. The Einasto profile with index n approximate to 6 is a stationary solution of the Fokker-Planck equation in the halo center. There are some reasons to believe that the solution is an attractor. Then the Fokker-Planck diffusion tends to transform a density profile to the equilibrium one with the Einasto index n approximate to 6. We suggest this effect as a possible reason why the Einasto index n approximate to 6 occurs so frequently in the interpretation of N-body simulation results. The results obtained cast doubt on generally accepted criteria of N-body simulation convergence. KW - dark matter theory KW - dwarfs galaxies KW - galaxy evolution KW - rotation curves of galaxies Y1 - 2018 U6 - https://doi.org/10.1088/1475-7516/2018/03/034 SN - 1475-7516 IS - 3 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Hani, Maan H. A1 - Sparre, Martin A1 - Ellison, Sara L. A1 - Torrey, Paul A1 - Vogelsberger, Mark T1 - Galaxy mergers moulding the circum-galactic medium BT - I. The impact of a major merger JF - Monthly notices of the Royal Astronomical Society N2 - Galaxies are surrounded by sizeable gas reservoirs which host a significant amount of metals: the circum-galactic medium (CGM). The CGM acts as a mediator between the galaxy and the extragalactic medium. However, our understanding of how galaxy mergers, a major evolutionary transformation, impact the CGM remains deficient. We present a theoretical study of the effect of galaxy mergers on the CGM. We use hydrodynamical cosmological zoom-in simulations of a major merger selected from the Illustris project such that the z = 0 descendant has a halo mass and stellar mass comparable to the Milky Way. To study the CGM we then re-simulated this system at a 40 times better mass resolution, and included detailed post-processing ionization modelling. Our work demonstrates the effect the merger has on the characteristic size of the CGM, its metallicity, and the predicted covering fraction of various commonly observed gas-phase species, such as H I, C IV, and O VI. We show that merger-induced outflows can increase the CGM metallicity by 0.2-0.3 dex within 0.5 Gyr post-merger. These effects last up to 6 Gyr post-merger. While the merger increases the total metal covering fractions by factors of 2-3, the covering fractions of commonly observed UV ions decrease due to the hard ionizing radiation from the active galactic nucleus, which we model explicitly. Our study of the single simulated major merger presented in this work demonstrates the significant impact that a galaxy interaction can have on the size, metallicity, and observed column densities of the CGM. KW - methods: numerical KW - galaxies: evolution KW - galaxies: haloes KW - galaxies: interactions Y1 - 2017 U6 - https://doi.org/10.1093/mnras/stx3252 SN - 0035-8711 SN - 1365-2966 VL - 475 IS - 1 SP - 1160 EP - 1176 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Uola, Roope A1 - Lever, Fabiano A1 - Gühne, Otfried A1 - Pellonpaa, Juha-Pekka T1 - Unified picture for spatial, temporal, and channel steering JF - Physical review : A, Atomic, molecular, and optical physics N2 - Quantum steering describes how local actions on a quantum system can affect another, spacelike separated, quantum state. Lately, quantum steering has been formulated also for timelike scenarios and for quantum channels. We approach all the three scenarios as one using tools from Stinespring dilations of quantum channels. By applying our technique we link all three steering problems one-to-one with the incompatibility of quantum measurements, a result formerly known only for spatial steering. We exploit this connection by showing how measurement uncertainty relations can be used as tight steering inequalities for all three scenarios. Moreover, we show that certain notions of temporal and spatial steering are fully equivalent and prove a hierarchy between temporal steering and macrorealistic hidden variable models. Y1 - 2018 U6 - https://doi.org/10.1103/PhysRevA.97.032301 SN - 2469-9926 SN - 2469-9934 VL - 97 IS - 3 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Goychuk, Igor T1 - Sensing magnetic fields with magnetosensitive ion channels JF - Sensors N2 - Magnetic nanoparticles are met across many biological species ranging from magnetosensitive bacteria, fishes, bees, bats, rats, birds, to humans. They can be both of biogenetic origin and due to environmental contamination, being either in paramagnetic or ferromagnetic state. The energy of such naturally occurring single-domain magnetic nanoparticles can reach up to 10-20 room k(B)T in the magnetic field of the Earth, which naturally led to supposition that they can serve as sensory elements in various animals. This work explores within a stochastic modeling framework a fascinating hypothesis of magnetosensitive ion channels with magnetic nanoparticles serving as sensory elements, especially, how realistic it is given a highly dissipative viscoelastic interior of living cells and typical sizes of nanoparticles possibly involved. KW - magnetic nanoparticles KW - ion channels KW - viscoelastic effects and anomalous diffusion KW - non-exponential statistics KW - influence of weak magnetic fields on living systems Y1 - 2018 U6 - https://doi.org/10.3390/s18030728 SN - 1424-8220 VL - 18 IS - 3 PB - MDPI CY - Basel ER - TY - GEN A1 - Parsons, R. D. A1 - Schüssler, F. A1 - Garrigoux, T. A1 - Balzer, A. A1 - Füssling, Matthias A1 - Hoischen, Clemens A1 - Holler, M. A1 - Mitchell, A. A1 - Pühlhofer, G. A1 - Rowell, G. A1 - Wagner, S. A1 - Bissaldi, E. A1 - Tam, P. H. T. T1 - The HESS II GRB Observation Scheme T2 - AIP conference proceedings / American Institute of Physics N2 - Gamma-ray bursts (GRBs) are some of the Universe’s most enigmatic and exotic events. However, at energies above 10 GeV their behaviour remains largely unknown. Although space based telescopes such as the Fermi-LAT have been able to detect GRBs in this energy range, their photon statistics are limited by the small detector size. Such limitations are not present in ground based gamma-ray telescopes such as the H.E.S.S. experiment, which has now entered its second phase with the addition of a large 600 m2 telescope to the centre of the array. Such a large telescope allows H.E.S.S. to access the sub 100-GeV energy range while still maintaining a large effective collection area, helping to potentially probe the short timescale emission of these events. We present a description of the H.E.S.S. GRB observation programme, summarising the performance of the rapid GRB repointing system and the conditions under which GRB observations are initiated. Additionally we will report on the GRB follow-ups made during the 2014-15 observation campaigns. Y1 - 2017 SN - 978-0-7354-1456-3 U6 - https://doi.org/10.1063/1.4968980 SN - 0094-243X SN - 1551-7616 VL - 1792 IS - 1 PB - American Institute of Physics CY - Melville ER - TY - GEN A1 - Angüner, Ekrem Oǧuzhan A1 - Aharonian, Felix A. A1 - Bordas, Pol A1 - Casanova, Sabrina A1 - Hoischen, Clemens A1 - Oya, I. A1 - Ziegler, A. T1 - HESS J1826-130 BT - a very hard gamma-Ray spectrum source in the Galactic Plane T2 - AIP conference proceedings / American Institute of Physics N2 - HESS J1826-130 is an unidentified hard spectrum source discovered by H.E.S.S. along the Galactic plane, the spectral index being Gamma = 1.6 with an exponential cut-off at about 12 TeV. While the source does not have a clear counterpart at longer wavelengths, the very hard spectrum emission at TeV energies implies that electrons or protons accelerated up to several hundreds of TeV are responsible for the emission. In the hadronic case, the VHE emission can be produced by runaway cosmic-rays colliding with the dense molecular clouds spatially coincident with the H.E.S.S. source. Y1 - 2017 SN - 978-0-7354-1456-3 U6 - https://doi.org/10.1063/1.4968928 SN - 0094-243X SN - 1551-7616 VL - 1792 IS - 1 PB - American Institute of Physics CY - Melville ER - TY - JOUR A1 - Metzler, Ralf T1 - Superstatistics and non-Gaussian diffusion JF - The European physical journal special topics N2 - Brownian motion and viscoelastic anomalous diffusion in homogeneous environments are intrinsically Gaussian processes. In a growing number of systems, however, non-Gaussian displacement distributions of these processes are being reported. The physical cause of the non-Gaussianity is typically seen in different forms of disorder. These include, for instance, imperfect "ensembles" of tracer particles, the presence of local variations of the tracer mobility in heteroegenous environments, or cases in which the speed or persistence of moving nematodes or cells are distributed. From a theoretical point of view stochastic descriptions based on distributed ("superstatistical") transport coefficients as well as time-dependent generalisations based on stochastic transport parameters with built-in finite correlation time are invoked. After a brief review of the history of Brownian motion and the famed Gaussian displacement distribution, we here provide a brief introduction to the phenomenon of non-Gaussianity and the stochastic modelling in terms of superstatistical and diffusing-diffusivity approaches. KW - Brownian diffusion KW - anomalous diffusion KW - dynamics KW - kinetic-theory KW - models KW - motion KW - nanoparticles KW - nonergodicity KW - statistics KW - subdiffusion Y1 - 2020 U6 - https://doi.org/10.1140/epjst/e2020-900210-x SN - 1951-6355 SN - 1951-6401 VL - 229 IS - 5 SP - 711 EP - 728 PB - Springer CY - Heidelberg ER - TY - JOUR A1 - Abdalla, Hassan E. A1 - Adam, Remi A1 - Aharonian, Felix A. A1 - Benkhali, Faical Ait A1 - Angüner, Ekrem Oǧuzhan A1 - Arakawa, Masanori A1 - Arcaro, C A1 - Armand, Catherine A1 - Armstrong, T. A1 - Egberts, Kathrin T1 - Very high energy γ-ray emission from two blazars of unknown redshift and upper limits on their distance JF - Monthly Notices of the Royal Astronomical Society N2 - We report on the detection of very high energy (VHE; E > 100 GeV) gamma-ray emission from the BL Lac objects KUV 00311-1938 and PKS 1440-389 with the High Energy Stereoscopic System (H.E.S.S.). H.E.S.S. observations were accompanied or preceded by multiwavelength observations with Fermi/LAT, XRT and UVOT onboard the Swift satellite, and ATOM. Based on an extrapolation of the Fermi/LAT spectrum towards the VHE gamma-ray regime, we deduce a 95 per cent confidence level upper limit on the unknown redshift of KUV 00311-1938 of z < 0.98 and of PKS 1440-389 of z < 0.53. When combined with previous spectroscopy results, the redshift of KUV 00311-1938 is constrained to 0.51 <= z < 0.98 and of PKS 1440-389 to 0.14 (sic) z < 0.53. KW - BL Lacertae objects: individual KW - galaxies: high-redshift KW - gamma-rays: general KW - Resolved and unresolved sources as a function of wavelength Y1 - 2020 VL - 494 IS - 4 PB - Wiley-Blackwell CY - Oxford ER - TY - JOUR A1 - Teichmann, Erik T1 - Using phase dynamics to study partial synchrony BT - three examples JF - European physical journal special topics N2 - Partial synchronous states appear between full synchrony and asynchrony and exhibit many interesting properties. Most frequently, these states are studied within the framework of phase approximation. The latter is used ubiquitously to analyze coupled oscillatory systems. Typically, the phase dynamics description is obtained in the weak coupling limit, i.e., in the first-order in the coupling strength. The extension beyond the first-order represents an unsolved problem and is an active area of research. In this paper, three partially synchronous states are investigated and presented in order of increasing complexity. First, the usage of the phase response curve for the description of macroscopic oscillators is analyzed. To achieve this, the response of the mean-field oscillations in a model of all-to-all coupled limit-cycle oscillators to pulse stimulation is measured. The next part treats a two-group Kuramoto model, where the interaction of one attractive and one repulsive group results in an interesting solitary state, situated between full synchrony and self-consistent partial synchrony. In the last part, the phase dynamics of a relatively simple system of three Stuart-Landau oscillators are extended beyond the weak coupling limit. The resulting model contains triplet terms in the high-order phase approximation, though the structural connections are only pairwise. Finally, the scaling of the new terms with the coupling is analyzed. Y1 - 2021 U6 - https://doi.org/10.1140/epjs/s11734-021-00156-3 SN - 1951-6355 SN - 1951-6401 VL - 230 IS - 14-15 SP - 2833 EP - 2842 PB - Springer CY - Heidelberg ER - TY - JOUR A1 - Schirdewahn, Daniel T1 - Stability of a parametric harmonic oscillator with dichotomic noise JF - Chaos : an interdisciplinary journal of nonlinear science N2 - The harmonic oscillator is a powerful model that can appear as a limit case when examining a nonlinear system. A well known fact is that, without driving, the inclusion of a friction term makes the origin of the phase space-which is a fixed point of the system-linearly stable. In this work, we include a telegraph process as perturbation of the oscillator's frequency, for example, to describe the motion of a particle with fluctuating charge gyrating in an external magnetic field. Increasing intensity of this colored noise is capable of changing the quality of the fixed point. To characterize the stability of the system, we use a stability measure that describes the growth of the displacement of the system's phase space position and express it in a closed form. We expand the respective exponent for light friction and low noise intensity and compare both the exact analytic solution and the expansion to numerical values. Our findings allow stability predictions for several physical systems. Y1 - 2020 U6 - https://doi.org/10.1063/5.0012946 SN - 1054-1500 SN - 1089-7682 VL - 30 IS - 9 PB - American Institute of Physics CY - Melville ER - TY - JOUR A1 - Rosenblum, Michael T1 - Controlling collective synchrony in oscillatory ensembles by precisely timed pulses JF - Chaos : an interdisciplinary journal of nonlinear science N2 - We present an efficient technique for control of synchrony in a globally coupled ensemble by pulsatile action. We assume that we can observe the collective oscillation and can stimulate all elements of the ensemble simultaneously. We pay special attention to the minimization of intervention into the system. The key idea is to stimulate only at the most sensitive phase. To find this phase, we implement an adaptive feedback control. Estimating the instantaneous phase of the collective mode on the fly, we achieve efficient suppression using a few pulses per oscillatory cycle. We discuss the possible relevance of the results for neuroscience, namely, for the development of advanced algorithms for deep brain stimulation, a medical technique used to treat Parkinson's disease. Y1 - 2020 U6 - https://doi.org/10.1063/5.0019823 SN - 1054-1500 SN - 1089-7682 VL - 30 IS - 9 PB - American Institute of Physics CY - Melville ER - TY - JOUR A1 - Beta, Carsten A1 - Kruse, Karsten T1 - Intracellular oscillations and waves JF - Annual review of condensed matter physics N2 - Dynamic processes in living cells are highly organized in space and time. Unraveling the underlying molecular mechanisms of spatiotemporal pattern formation remains one of the outstanding challenges at the interface between physics and biology. A fundamental recurrent pattern found in many different cell types is that of self-sustained oscillations. They are involved in a wide range of cellular functions, including second messenger signaling, gene expression, and cytoskeletal dynamics. Here, we review recent developments in the field of cellular oscillations and focus on cases where concepts from physics have been instrumental for understanding the underlying mechanisms. We consider biochemical and genetic oscillators as well as oscillations that arise from chemo-mechanical coupling. Finally, we highlight recent studies of intracellular waves that have increasingly moved into the focus of this research field. KW - self-sustained oscillations KW - biochemical oscillators KW - genetic networks KW - chemomechanical coupling KW - actin waves Y1 - 2017 SN - 978-0-8243-5008-6 U6 - https://doi.org/10.1146/annurev-conmatphys-031016-025210 SN - 1947-5454 VL - 8 SP - 239 EP - 264 PB - Annual Reviews CY - Palo Alto ER - TY - THES A1 - Müller, Melanie J. I. T1 - Bidirectional transport by molecular motors T1 - Bidirektionaler Transport durch molekulare Motoren N2 - In biological cells, the long-range intracellular traffic is powered by molecular motors which transport various cargos along microtubule filaments. The microtubules possess an intrinsic direction, having a 'plus' and a 'minus' end. Some molecular motors such as cytoplasmic dynein walk to the minus end, while others such as conventional kinesin walk to the plus end. Cells typically have an isopolar microtubule network. This is most pronounced in neuronal axons or fungal hyphae. In these long and thin tubular protrusions, the microtubules are arranged parallel to the tube axis with the minus ends pointing to the cell body and the plus ends pointing to the tip. In such a tubular compartment, transport by only one motor type leads to 'motor traffic jams'. Kinesin-driven cargos accumulate at the tip, while dynein-driven cargos accumulate near the cell body. We identify the relevant length scales and characterize the jamming behaviour in these tube geometries by using both Monte Carlo simulations and analytical calculations. A possible solution to this jamming problem is to transport cargos with a team of plus and a team of minus motors simultaneously, so that they can travel bidirectionally, as observed in cells. The presumably simplest mechanism for such bidirectional transport is provided by a 'tug-of-war' between the two motor teams which is governed by mechanical motor interactions only. We develop a stochastic tug-of-war model and study it with numerical and analytical calculations. We find a surprisingly complex cooperative motility behaviour. We compare our results to the available experimental data, which we reproduce qualitatively and quantitatively. N2 - In biologischen Zellen transportieren molekulare Motoren verschiedenste Frachtteilchen entlang von Mikrotubuli-Filamenten. Die Mikrotubuli-Filamente besitzen eine intrinsische Richtung: sie haben ein "Plus-" und ein "Minus-"Ende. Einige molekulare Motoren wie Dynein laufen zum Minus-Ende, während andere wie Kinesin zum Plus-Ende laufen. Zellen haben typischerweise ein isopolares Mikrotubuli-Netzwerk. Dies ist besonders ausgeprägt in neuronalen Axonen oder Pilz-Hyphen. In diesen langen röhrenförmigen Ausstülpungen liegen die Mikrotubuli parallel zur Achse mit dem Minus-Ende zum Zellkörper und dem Plus-Ende zur Zellspitze gerichtet. In einer solchen Röhre führt Transport durch nur einen Motor-Typ zu "Motor-Staus". Kinesin-getriebene Frachten akkumulieren an der Spitze, während Dynein-getriebene Frachten am Zellkörper akkumulieren. Wir identifizieren die relevanten Längenskalen und charakterisieren das Stauverhalten in diesen Röhrengeometrien mit Hilfe von Monte-Carlo-Simulationen und analytischen Rechnungen. Eine mögliche Lösung für das Stauproblem ist der Transport mit einem Team von Plus- und einem Team von Minus-Motoren gleichzeitig, so dass die Fracht sich in beide Richtungen bewegen kann. Dies wird in Zellen tatsächlich beobachtet. Der einfachste Mechanismus für solchen bidirektionalen Transport ist ein "Tauziehen" zwischen den beiden Motor-Teams, das nur mit mechanischer Interaktion funktioniert. Wir entwickeln ein stochastisches Tauzieh-Modell, das wir mit numerischen und analytischen Rechnungen untersuchen. Es ergibt sich ein erstaunlich komplexes Motilitätsverhalten. Wir vergleichen unsere Resultate mit den vorhandenen experimentellen Daten, die wir qualitativ und quantitativ reproduzieren. KW - molekulare Motoren KW - bidirektionaler intrazellulärer Transport KW - Tauziehen KW - stochastische Prozesse KW - kooperative Phänomene KW - molecular motors KW - bidirectional intracellular transport KW - tug-of-war KW - stochastic processes KW - cooperative phenomena Y1 - 2008 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-18715 ER - TY - JOUR A1 - Rubio, Jesús A1 - Anders, Janet A1 - Correa, Luis A. T1 - Global quantum thermometry JF - Physical review letters / publ. by the American Physical Society N2 - A paradigm shift in quantum thermometry is proposed. To date, thermometry has relied on local estimation, which is useful to reduce statistical fluctuations once the temperature is very well known. In order to estimate temperatures in cases where few measurement data or no substantial prior knowledge are available, we build instead a method for global quantum thermometry. Based on scaling arguments, a mean logarithmic error is shown here to be the correct figure of merit for thermometry. Its full minimization provides an operational and optimal rule to postprocess measurements into a temperature reading, and it establishes a global precision limit. We apply these results to the simulated outcomes of measurements on a spin gas, finding that the local approach can lead to biased temperature estimates in cases where the global estimator converges to the true temperature. The global framework thus enables a reliable approach to data analysis in thermometry experiments. Y1 - 2021 U6 - https://doi.org/10.1103/PhysRevLett.127.190402 SN - 0031-9007 SN - 1079-7114 VL - 127 IS - 19 PB - American Physical Society CY - College Park ER - TY - THES A1 - Bachmann, Felix T1 - Non-linearity of magnetic micropropellers BT - chances and challenges of complex dynamics at the microscale Y1 - 2019 ER - TY - GEN A1 - Thoelert, Steffen A1 - Hörmann, Ulrich A1 - Antreich, Felix A1 - Meurer, Michael T1 - Ionospheric effects on high gain antenna GNSS measurements BT - TEC estimation and correction T2 - Proceedings of the 30th International Technical Meeting of the Satellite Division of The Institute of Navigation (ION GNSS+ 2017) N2 - The ionospheric delay of global navigation satellite systems (GNSS) signals typically is compensated by adding a single correction value to the pseudorange measurement of a GNSS receiver. Yet, this neglects the dispersive nature of the ionosphere. In this context we analyze the ionospheric signal distortion beyond a constant delay. These effects become increasingly significant with the signal bandwidth and hence more important for new broadband navigation signals. Using measurements of the Galileo E5 signal, captured with a high gain antenna, we verify that the expected influence can indeed be observed and compensated. A new method to estimate the total electron content (TEC) from a single frequency high gain antenna measurement of a broadband GNSS signal is proposed and described in detail. The received signal is de facto unaffected by multi-path and interference because of the narrow aperture angle of the used antenna which should reduce the error source of the result in general. We would like to point out that such measurements are independent of code correlation, like in standard receiver applications. It is therefore also usable without knowledge of the signal coding. Results of the TEC estimation process are shown and discussed comparing to common TEC products like TEC maps and dual frequency receiver estimates. Y1 - 2017 U6 - https://doi.org/10.33012/2017.15343 SN - 2331-5911 SN - 2331-5954 SP - 3368 EP - 3374 PB - Instituite of Navigation CY - Washington ER - TY - THES A1 - Avila, Gastón T1 - Asymptotic staticity and tensor decompositions with fast decay conditions T1 - Asymptotisch statische Anfangsdaten und Tensor-Zerlegungen mit starken Abfallbedingungen N2 - Corvino, Corvino and Schoen, Chruściel and Delay have shown the existence of a large class of asymptotically flat vacuum initial data for Einstein's field equations which are static or stationary in a neighborhood of space-like infinity, yet quite general in the interior. The proof relies on some abstract, non-constructive arguments which makes it difficult to calculate such data numerically by using similar arguments. A quasilinear elliptic system of equations is presented of which we expect that it can be used to construct vacuum initial data which are asymptotically flat, time-reflection symmetric, and asymptotic to static data up to a prescribed order at space-like infinity. A perturbation argument is used to show the existence of solutions. It is valid when the order at which the solutions approach staticity is restricted to a certain range. Difficulties appear when trying to improve this result to show the existence of solutions that are asymptotically static at higher order. The problems arise from the lack of surjectivity of a certain operator. Some tensor decompositions in asymptotically flat manifolds exhibit some of the difficulties encountered above. The Helmholtz decomposition, which plays a role in the preparation of initial data for the Maxwell equations, is discussed as a model problem. A method to circumvent the difficulties that arise when fast decay rates are required is discussed. This is done in a way that opens the possibility to perform numerical computations. The insights from the analysis of the Helmholtz decomposition are applied to the York decomposition, which is related to that part of the quasilinear system which gives rise to the difficulties. For this decomposition analogous results are obtained. It turns out, however, that in this case the presence of symmetries of the underlying metric leads to certain complications. The question, whether the results obtained so far can be used again to show by a perturbation argument the existence of vacuum initial data which approach static solutions at infinity at any given order, thus remains open. The answer requires further analysis and perhaps new methods. N2 - Corvino, Corvino und Schoen als auch Chruściel und Delay haben die Existenz einer grossen Klasse asymptotisch flacher Anfangsdaten für Einsteins Vakuumfeldgleichungen gezeigt, die in einer Umgebung des raumartig Unendlichen statisch oder stationär aber im Inneren der Anfangshyperfläche sehr allgemein sind. Der Beweis beruht zum Teil auf abstrakten, nicht konstruktiven Argumenten, die Schwierigkeiten bereiten, wenn derartige Daten numerisch berechnet werden sollen. In der Arbeit wird ein quasilineares elliptisches Gleichungssystem vorgestellt, von dem wir annehmen, dass es geeignet ist, asymptotisch flache Vakuumanfangsdaten zu berechnen, die zeitreflektionssymmetrisch sind und im raumartig Unendlichen in einer vorgeschriebenen Ordnung asymptotisch zu statischen Daten sind. Mit einem Störungsargument wird ein Existenzsatz bewiesen, der gilt, solange die Ordnung, in welcher die Lösungen asymptotisch statische Lösungen approximieren, in einem gewissen eingeschränkten Bereich liegt. Versucht man, den Gültigkeitsbereich des Satzes zu erweitern, treten Schwierigkeiten auf. Diese hängen damit zusammen, dass ein gewisser Operator nicht mehr surjektiv ist. In einigen Tensorzerlegungen auf asymptotisch flachen Räumen treten ähnliche Probleme auf, wie die oben erwähnten. Die Helmholtzzerlegung, die bei der Bereitstellung von Anfangsdaten für die Maxwellgleichungen eine Rolle spielt, wird als ein Modellfall diskutiert. Es wird eine Methode angegeben, die es erlaubt, die Schwierigkeiten zu umgehen, die auftreten, wenn ein schnelles Abfallverhalten des gesuchten Vektorfeldes im raumartig Unendlichen gefordert wird. Diese Methode gestattet es, solche Felder auch numerisch zu berechnen. Die Einsichten aus der Analyse der Helmholtzzerlegung werden dann auf die Yorkzerlegung angewandt, die in den Teil des quasilinearen Systems eingeht, der Anlass zu den genannten Schwierigkeiten gibt. Für diese Zerlegung ergeben sich analoge Resultate. Es treten allerdings Schwierigkeiten auf, wenn die zu Grunde liegende Metrik Symmetrien aufweist. Die Frage, ob die Ergebnisse, die soweit erhalten wurden, in einem Störungsargument verwendet werden können um die Existenz von Vakuumdaten zu zeigen, die im räumlich Unendlichen in jeder Ordnung statische Daten approximieren, bleibt daher offen. Die Antwort erfordert eine weitergehende Untersuchung und möglicherweise auch neue Methoden. KW - Einsteins Feldgleichungen KW - Zwangsgleichungen KW - Tensor-Zerlegungen KW - raumartige Unendliche KW - elliptisches Gleichungssystem KW - Einstein's field equations KW - constraint equations KW - tensor decompositions KW - space-like infinity KW - elliptic systems Y1 - 2011 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-54046 ER - TY - THES A1 - Winkler, Michael T1 - Thinning and turbulence in aqueous films N2 - This thesis covers the topic ”Thinning and Turbulence in Aqueous Films”. Experimental studies in two-dimensional systems gained an increasing amount of attention during the last decade. Thin liquid films serve as paradigms of atmospheric convection, thermal convection in the Earth’s mantle or turbulence in magnetohydrodynamics. Recent research on colloids, interfaces and nanofluids lead to advances in the developtment of micro-mixers (lab-on-a-chip devices). In this project a detailed description of a thin film experiment with focus on the particular surface forces is presented. The impact of turbulence on the thinning of liquid films which are oriented parallel to the gravitational force is studied. An experimental setup was developed which permits the capturing of thin film interference patterns under controlled surface and atmospheric conditions. The measurement setup also serves as a prototype of a mixer on the basis of thermally induced turbulence in liquid thin films with thicknesses in the nanometer range. The convection is realized by placing a cooled copper rod in the center of the film. The temperature gradient between the rod and the atmosphere results in a density gradient in the liquid film, so that different buoyancies generate turbulence. In the work at hand the thermally driven convection is characterized by a newly developed algorithm, named Cluster Imaging Velocimetry (CIV). This routine determines the flow relevant vector fields (velocity and deformation). On the basis of these insights the flow in the experiment was investigated with respect to its mixing properties. The mixing characteristics were compared to theoretical models and mixing efficiency of the flow scheme calculated. The gravitationally driven thinning of the liquid film was analyzed under the influence of turbulence. Strong shear forces lead to the generation of ultra-thin domains which consist of Newton black film. Due to the exponential expansion of the thin areas and the efficient mixing, this two-phase flow rapidly turns into the convection of only ultra-thin film. This turbulence driven transition was observed and quantified for the first time. The existence of stable convection in liquid nanofilms was proven for the first time in the context of this work. N2 - Diese Diplomarbeit behandelt das Thema ”Dünnung und Turbulenz in wässrigen Filmen”. Experimente in zweidimensionalen Systemen erfuhren in den vergangenen Jahren zunehmend an Aufmerksamkeit. Dünne Flüssigkeitsschichten dienen als Modell für atmosphärische Konvektion, thermische Konvektion im Erdmantel oder Turbulenz in der Magnetohydrodynamik. Aktuelle Forschung im Bereich der Kolloide, Grenzflächen und Nanofluidik führt zu Fortschritten in der Entwicklung von Mikromixern (”lab-on-a-chip”). In diesem Projekt wird eine detaillierte Beschreibung eines Dünnfilmexperiments mit Fokus auf die besonderen Oberflächenkräfte vorgestellt. Die Auswirkung der Turbulenz auf die Dünnung von parallel zur Gravitationskraft orientierten Flüssigkeitsschichten wurde untersucht. Es wurde ein Experiment entwickelt, welches die Aufnahme von Dünnschichtinterferenzmustern unter kontrollierten Oberflächenbedingungen und Atmosphäre erlaubt. Der Messaufbau dient auch als Prototyp eines Mixers auf Basis von thermisch induzierter Turbulenz in Flüssigkeitsfilmen mit Dicken im Nanometerbereich. Die Konvektion wird durch das Platzieren eines gekühlten Kupferstabs in der Mitte des Films realisiert. Der Temperaturgradient zwischen Stab und äußerer Atmosphäre resultiert in einem Dichtegradienten in dem flüssigen Film, sodass durch unterschiedliche Auftriebskräfte Turbulenz erzeugt wird. In der vorliegenden Arbeit ist die thermisch getriebenen Konvektion an Hand eines neu entwickelten Verfahrens (Cluster Imaging Velocimetry - CIV) zur Ermittlung des strömungsrelevanten Vektorfelder (Geschwindigkeit und Deformation) charakterisiert worden. Auf Basis dieser Erkenntnisse wurde die im Experiment vorherrschende Strömung in Hinsicht auf ihre Mischungseigenschaften im Vergleich zu theoretischen Modellen untersucht und die Mischungseffizienz berechnet. Die gravitationsgetriebene Ausdünnung der Flüssigkeitsschicht unter Einfluss der Turbulenz wurde analysiert. Durch starke Scherkräfte kommt es lokal zur Bildung ultradünner Domänen bestehend aus ”Newton black film”. Diese Zweiphasenströmung geht durch das exponentielle Ausdehnen der dünnen Bereiche und die effiziente Mischung sehr schnell in eine Konvektion von ausschließlich ultradünnem Film im Gleichgewichtszustand über. Dieser turbulenzgetriebene Übergang wurde zum ersten Mal beobachtet und quantifiziert. Die Existenz stabiler Konvektion in flüssigen Nanofilmen ist zum ersten Mal im Rahmen dieser Arbeit belegt worden. KW - wässrige Filme KW - Nanofluid KW - Mischung KW - Konvektion KW - Dünnung KW - Thin Film KW - Nanofluid KW - Mixing KW - Convection KW - Rapid thinning Y1 - 2011 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-53107 ER - TY - THES A1 - Malik, Nishant T1 - Extremes in events and dynamics : a nonlinear data analysis perspective on the past and present dynamics of the Indian summer monsoon N2 - To identify extreme changes in the dynamics of the Indian Summer Monsoon (ISM) in the past, I propose a new approach based on the quantification of fluctuations of a nonlinear similarity measure, to identify regimes of distinct dynamical complexity in short time series. I provide an analytical derivation for the relationship of the new measure with the dynamical invariants such as dimension and Lyapunov exponents of the underlying system. A statistical test is also developed to estimate the significance of the identified transitions. Our method is justified by uncovering bifurcation structures in several paradigmatic models, providing more complex transitions compared with traditional Lyapunov exponents. In a real world situation, we apply the method to identify millennial-scale dynamical transitions in Pleistocene proxy records of the south Asian summer monsoon system. We infer that many of these transitions are induced by the external forcing of solar insolation and are also affected by internal forcing on Monsoonal dynamics, i.e., the glaciation cycles of the Northern Hemisphere and the onset of the tropical Walker circulation. Although this new method has general applicability, it is particularly useful in analysing short palaeo-climate records. Rainfall during the ISM over the Indian subcontinent occurs in form of enormously complex spatiotemporal patterns due to the underlying dynamics of atmospheric circulation and varying topography. I present a detailed analysis of summer monsoon rainfall over the Indian peninsular using Event Synchronization (ES), a measure of nonlinear correlation for point processes such as rainfall. First, using hierarchical clustering I identify principle regions where the dynamics of monsoonal rainfall is more coherent or homogenous. I also provide a method to reconstruct the time delay patterns of rain events. Moreover, further analysis is carried out employing the tools of complex network theory. This study provides valuable insights into the spatial organization, scales, and structure of the 90th and 94th percentile rainfall events during the ISM (June to September). I furthermore analyse the influence of different critical synoptic atmospheric systems and the impact of the steep Himalayan topography on rainfall patterns. The presented method not only helps in visualising the structure of the extremeevent rainfall fields, but also identifies the water vapor pathways and decadal-scale moisture sinks over the region. Furthermore a simple scheme based on complex networks is presented to decipher the spatial intricacies and temporal evolution of monsoonal rainfall patterns over the last six decades. Some supplementary results on the evolution of monsoonal rainfall extremes over the last sixty years are also presented. N2 - Um Extremereignisse in der Dynamik des indischen Sommermonsuns (ISM) in der geologischen Vergangenheit zu identifizieren, schlage ich einen neuartigen Ansatz basierend auf der Quantifikation von Fluktuationen in einem nichtlinearen Ähnlichkeitsmaß vor. Dieser reagiert empfindlich auf Zeitabschnitte mit deutlichen Veränderungen in der dynamischen Komplexität kurzer Zeitreihen. Ein mathematischer Zusammenhang zwischen dem neuen Maß und dynamischen Invarianten des zugrundeliegenden Systems wie fraktalen Dimensionen und Lyapunovexponenten wird analytisch hergeleitet. Weiterhin entwickle ich einen statistischen Test zur Schätzung der Signifikanz der so identifizierten dynamischen Übergänge. Die Stärken der Methode werden durch die Aufdeckung von Bifurkationsstrukturen in paradigmatischen Modellsystemen nachgewiesen, wobei im Vergleich zu den traditionellen Lyapunovexponenten eine Identifikation komplexerer dynamischer Übergänge möglich ist. Wir wenden die neu entwickelte Methode zur Analyse realer Messdaten an, um ausgeprägte dynamische Veränderungen auf Zeitskalen von Jahrtausenden in Klimaproxydaten des südasiatischen Sommermonsunsystems während des Pleistozäns aufzuspüren. Dabei zeigt sich, dass viele dieser Übergänge durch den externen Einfluss der veränderlichen Sonneneinstrahlung, sowie durch dem Klimasystem interne Einflussfaktoren auf das Monsunsystem (Eiszeitzyklen der nördlichen Hemisphäre und Einsatz der tropischenWalkerzirkulation) induziert werden. Trotz seiner Anwendbarkeit auf allgemeine Zeitreihen ist der diskutierte Ansatz besonders zur Untersuchung von kurzen Paläoklimazeitreihen geeignet. Die während des ISM über dem indischen Subkontinent fallenden Niederschläge treten, bedingt durch die zugrundeliegende Dynamik der atmosphärischen Zirkulation und topographische Einflüsse, in äußerst komplexen, raumzeitlichen Mustern auf. Ich stelle eine detaillierte Analyse der Sommermonsunniederschläge über der indischen Halbinsel vor, die auf Ereignissynchronisation (ES) beruht, einem Maß für die nichtlineare Korrelation von Punktprozessen wie Niederschlagsereignissen. Mit hierarchischen Clusteringalgorithmen identifiziere ich zunächst Regionen mit besonders kohärenten oder homogenen Monsunniederschlägen. Dabei können auch die Zeitverzögerungsmuster von Regenereignissen rekonstruiert werden. Darüber hinaus führe ich weitere Analysen auf Basis der Theorie komplexer Netzwerke durch. Diese Studien ermöglichen wertvolle Einsichten in räumliche Organisation, Skalen und Strukturen von starken Niederschlagsereignissen oberhalb der 90% und 94% Perzentilen während des ISM (Juni bis September). Weiterhin untersuche ich den Einfluss von verschiedenen, kritischen synoptischen Systemen der Atmosphäre sowie der steilen Topographie des Himalayas auf diese Niederschlagsmuster. Die vorgestellte Methode ist nicht nur geeignet, die Struktur extremer Niederschlagsereignisse zu visualisieren, sondern kann darüber hinaus über der Region atmosphärische Transportwege von Wasserdampf und Feuchtigkeitssenken auf dekadischen Skalen identifizieren.Weiterhin wird ein einfaches, auf komplexen Netzwerken basierendes Verfahren zur Entschlüsselung der räumlichen Feinstruktur und Zeitentwicklung von Monsunniederschlagsextremen während der vergangenen 60 Jahre vorgestellt. T2 - Extrema in Ereignissen und Dynamiken : historische und heutige Dynamik des Indischen Sommer-Monsuns aus der Perspektive nichtlinearer Datenanalyse KW - nichtlineare Datenanalyse KW - Paläoklimatologie KW - Indischer Sommer-Monsun KW - Extremereignisse KW - komplexe Netzwerke KW - nonlinear time series analysis KW - Paleoclimatology KW - Indian summer monsoon KW - extreme events KW - complex networks Y1 - 2011 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-58016 ER - TY - THES A1 - Fischer, Jost T1 - Über Synchronisationsphänomene nichtlinearer akustischer Oszillatoren T1 - About synchronization phenomena of nonlinear acoustic oscillators N2 - In dieser Arbeit werden die Effekte der Synchronisation nichtlinearer, akustischer Oszillatoren am Beispiel zweier Orgelpfeifen untersucht. Aus vorhandenen, experimentellen Messdaten werden die typischen Merkmale der Synchronisation extrahiert und dargestellt. Es folgt eine detaillierte Analyse der Übergangsbereiche in das Synchronisationsplateau, der Phänomene während der Synchronisation, als auch das Austreten aus der Synchronisationsregion beider Orgelpfeifen, bei verschiedenen Kopplungsstärken. Die experimentellen Befunde werfen Fragestellungen nach der Kopplungsfunktion auf. Dazu wird die Tonentstehung in einer Orgelpfeife untersucht. Mit Hilfe von numerischen Simulationen der Tonentstehung wird der Frage nachgegangen, welche fluiddynamischen und aero-akustischen Ursachen die Tonentstehung in der Orgelpfeife hat und inwiefern sich die Mechanismen auf das Modell eines selbsterregten akustischen Oszillators abbilden lässt. Mit der Methode des Coarse Graining wird ein Modellansatz formuliert. N2 - In this study, synchronization properties observed in a system of nonlinear acoustic oscillators in form of two coupled organ pipes are investigated. From given measurements we extract the effects of synchronization one would expect typically. Furthermore we set our focus to the domains of transition into the synchronization region, when the system is complete synchronized and when it tears off, under the condition of different coupling strengths. We analyze and discuss the observed phenomena concerning their nonlinearities. Using numerical, fluid-dynamic and aeroacoustic simulation techniques we investigate how an organ pipe can be understand as a self-sustained, acoustic oscillator. With the results of the numerical simulations we show, how to reduce the complex fluid-dynamical interplay with the acoustic field inside the pipe to a self-sustained acoustic oscillator. For this process we use the coarse graining method. KW - Physik KW - Synchronisation KW - Orgelpfeife KW - nichtlinear KW - Akustik KW - physics KW - synchronization KW - organ pipe KW - nonlinear KW - acoustics Y1 - 2012 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-63618 ER - TY - THES A1 - Orgis, Thomas T1 - Unstetige Galerkin-Diskretisierung niedriger Ordnung in einem atmosphärischen Multiskalenmodell T1 - Low-order discontinuous Galerkin discretization in an atmospheric multi-scale model N2 - Die Dynamik der Atmosphäre der Erde umfasst einen Bereich von mikrophysikalischer Turbulenz über konvektive Prozesse und Wolkenbildung bis zu planetaren Wellenmustern. Für Wettervorhersage und zur Betrachtung des Klimas über Jahrzehnte und Jahrhunderte ist diese Gegenstand der Modellierung mit numerischen Verfahren. Mit voranschreitender Entwicklung der Rechentechnik sind Neuentwicklungen der dynamischen Kerne von Klimamodellen, die mit der feiner werdenden Auflösung auch entsprechende Prozesse auflösen können, notwendig. Der dynamische Kern eines Modells besteht in der Umsetzung (Diskretisierung) der grundlegenden dynamischen Gleichungen für die Entwicklung von Masse, Energie und Impuls, so dass sie mit Computern numerisch gelöst werden können. Die vorliegende Arbeit untersucht die Eignung eines unstetigen Galerkin-Verfahrens niedriger Ordnung für atmosphärische Anwendungen. Diese Eignung für Gleichungen mit Wirkungen von externen Kräften wie Erdanziehungskraft und Corioliskraft ist aus der Theorie nicht selbstverständlich. Es werden nötige Anpassungen beschrieben, die das Verfahren stabilisieren, ohne sogenannte „slope limiter” einzusetzen. Für das unmodifizierte Verfahren wird belegt, dass es nicht geeignet ist, atmosphärische Gleichgewichte stabil darzustellen. Das entwickelte stabilisierte Modell reproduziert eine Reihe von Standard-Testfällen der atmosphärischen Dynamik mit Euler- und Flachwassergleichungen in einem weiten Bereich von räumlichen und zeitlichen Skalen. Die Lösung der thermischen Windgleichung entlang der mit den Isobaren identischen charakteristischen Kurven liefert atmosphärische Gleichgewichtszustände mit durch vorgegebenem Grundstrom einstellbarer Neigung zu(barotropen und baroklinen)Instabilitäten, die für die Entwicklung von Zyklonen wesentlich sind. Im Gegensatz zu früheren Arbeiten sind diese Zustände direkt im z-System(Höhe in Metern)definiert und müssen nicht aus Druckkoordinaten übertragen werden.Mit diesen Zuständen, sowohl als Referenzzustand, von dem lediglich die Abweichungen numerisch betrachtet werden, und insbesondere auch als Startzustand, der einer kleinen Störung unterliegt, werden verschiedene Studien der Simulation von barotroper und barokliner Instabilität durchgeführt. Hervorzuheben ist dabei die durch die Formulierung von Grundströmen mit einstellbarer Baroklinität ermöglichte simulationsgestützte Studie des Grades der baroklinen Instabilität verschiedener Wellenlängen in Abhängigkeit von statischer Stabilität und vertikalem Windgradient als Entsprechung zu Stabilitätskarten aus theoretischen Betrachtungen in der Literatur. N2 - The dynamics of the Earth’s atmosphere encompass a range from microphysical turbulence over convective processes and cloud formation up to planetary wave patterns. For weather forecasting and the investigation of climate over decades and centuries, these are subject to modelling with numerical methods. With progressing development of computer technology, re-development of the dynamical cores of climate models is in order to properly handle processes covered by the increasing resolution. The dynamical core of a model consists of the adaptation(discretization)of the basic equations for the dynamics of mass, energy and momentum for solving them numerically employing computers. The presented work investigates the applicability of a low-order Discontinuous Galerkin (DG) method for atmospheric applications. With equations that include external forces like gravitation and the Coriolis force, that is not given by theory. Necessary changes for stabilizing the method without resorting to slope limiters are presented. For the unmodified method, the basic inability to properly keep atmospheric balances is demonstrated. The developed stabilized model reproduces a set of standard test cases in a wide range of spatial and temporal scales. The solution of the termal wind equation along its characteristics curves, those being identical to the isobars, produces balanced atmospheric states with tunable (barotropic and baroclinic) instability via a prescribed zonal wind field. The constructed instability directly relates to the generation of cyclones. In contrast to earlier works, these balanced states are directly given in the z system (height in meters), without need for elaborate conversion from pressure coordinates. With these constructed states, both as reference state, the deviations from which being considered numerically, and as especially as initial condition subject to a small perturbation, several studies of barotropic and baroclinic instability are conducted via simulations. Particularily, the construction of steady states with configurable zonal flows of certain baroclinity facilitates a simulation-based study of baroclinic instability of differing wavelengths, depending on static stability and vertical wind gradient, in correspondence with stability maps from theoretical considerations in the literature. KW - Atmosphärenmodellierung KW - Unstetiges Galerkin-Verfahren KW - Multiskale KW - Barokline Instabilität KW - thermische Windgleichung KW - atmospheric modelling KW - discontinuous Galerkin method KW - multi-scale KW - baroclinic instability KW - thermal wind equation Y1 - 2014 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-70687 ER - TY - THES A1 - Theves, Matthias T1 - Bacterial motility and growth in open and confined environments T1 - Bacterial motility and growth in open and confined environments N2 - In the presence of a solid-liquid or liquid-air interface, bacteria can choose between a planktonic and a sessile lifestyle. Depending on environmental conditions, cells swimming in close proximity to the interface can irreversibly attach to the surface and grow into three-dimensional aggregates where the majority of cells is sessile and embedded in an extracellular polymer matrix (biofilm). We used microfluidic tools and time lapse microscopy to perform experiments with the polarly flagellated soil bacterium Pseudomonas putida (P. putida), a bacterial species that is able to form biofilms. We analyzed individual trajectories of swimming cells, both in the bulk fluid and in close proximity to a glass-liquid interface. Additionally, surface related growth during the early phase of biofilm formation was investigated. In the bulk fluid, P.putida shows a typical bacterial swimming pattern of alternating periods of persistent displacement along a line (runs) and fast reorientation events (turns) and cells swim with an average speed around 24 micrometer per second. We found that the distribution of turning angles is bimodal with a dominating peak around 180 degrees. In approximately six out of ten turning events, the cell reverses its swimming direction. In addition, our analysis revealed that upon a reversal, the cell systematically changes its swimming speed by a factor of two on average. Based on the experimentally observed values of mean runtime and rotational diffusion, we presented a model to describe the spreading of a population of cells by a run-reverse random walker with alternating speeds. We successfully recover the mean square displacement and, by an extended version of the model, also the negative dip in the directional autocorrelation function as observed in the experiments. The analytical solution of the model demonstrates that alternating speeds enhance a cells ability to explore its environment as compared to a bacterium moving at a constant intermediate speed. As compared to the bulk fluid, for cells swimming near a solid boundary we observed an increase in swimming speed at distances below d= 5 micrometer and an increase in average angular velocity at distances below d= 4 micrometer. While the average speed was maximal with an increase around 15% at a distance of d= 3 micrometer, the angular velocity was highest in closest proximity to the boundary at d=1 micrometer with an increase around 90% as compared to the bulk fluid. To investigate the swimming behavior in a confinement between two solid boundaries, we developed an experimental setup to acquire three-dimensional trajectories using a piezo driven objective mount coupled to a high speed camera. Results on speed and angular velocity were consistent with motility statistics in the presence of a single boundary. Additionally, an analysis of the probability density revealed that a majority of cells accumulated near the upper and lower boundaries of the microchannel. The increase in angular velocity is consistent with previous studies, where bacteria near a solid boundary were shown to swim on circular trajectories, an effect which can be attributed to a wall induced torque. The increase in speed at a distance of several times the size of the cell body, however, cannot be explained by existing theories which either consider the drag increase on cell body and flagellum near a boundary (resistive force theory) or model the swimming microorganism by a multipole expansion to account for the flow field interaction between cell and boundary. An accumulation of swimming bacteria near solid boundaries has been observed in similar experiments. Our results confirm that collisions with the surface play an important role and hydrodynamic interactions alone cannot explain the steady-state accumulation of cells near the channel walls. Furthermore, we monitored the number growth of cells in the microchannel under medium rich conditions. We observed that, after a lag time, initially isolated cells at the surface started to grow by division into colonies of increasing size, while coexisting with a comparable smaller number of swimming cells. After 5:50 hours, we observed a sudden jump in the number of swimming cells, which was accompanied by a breakup of bigger clusters on the surface. After approximately 30 minutes where planktonic cells dominated in the microchannel, individual swimming cells reattached to the surface. We interpret this process as an emigration and recolonization event. A number of complementary experiments were performed to investigate the influence of collective effects or a depletion of the growth medium on the transition. Similar to earlier observations on another bacterium from the same family we found that the release of cells to the swimming phase is most likely the result of an individual adaption process, where syntheses of proteins for flagellar motility are upregulated after a number of division cycles at the surface. N2 - Bakterien sind einzellige Mikroorganismen, die sich in flüssigem Medium mit Hilfe von rotierenden Flagellen, länglichen Fasern aus Proteinen, schwimmend fortbewegen. In Gegenwart einer Grenzfläche und unter günstigen Umweltbedingungen siedeln sich Bakterien an der Oberfläche an und gehen in eine sesshafte Wachstumsphase über. Die Wachstumsphase an der Oberfläche ist gekennzeichnet durch das Absondern von klebrigen, nährstoffreichen extrazellulären Substanzen, welche die Verbindung der Bakterien untereinander und mit der Oberfläche verstärken. Die entstehenden Aggregate aus extrazellulärer Matrix und Bakterien werden als Biofilm bezeichnet. In der vorliegenden Arbeit untersuchten wir ein Bodenbakterium, Pseudomonas putida (P. putida), welches in wässriger Umgebung an festen Oberflächen Biofilme ausbildet. Wir benutzten photolithographisch hergestellte Mikrokanäle und Hochgeschwindigkeits-Videomikroskopie um die Bewegung schwimmender Zellen in verschiedenen Abständen zu einer Glasoberfläche aufzunehmen. Zusätzlich wurden Daten über das parallel stattfindende Wachstum der sesshaften Zellen an der Oberfläche aufgezeichnet. Die Analyse von Trajektorien frei schwimmender Zellen zeigte, dass sich Liniensegmente, entlang derer sich die Zellen in eine konstante Richtung bewegen, mit scharfen Kehrtwendungen mit einem Winkel von 180 Grad abwechseln. Dabei änderte sich die Schwimmgeschwindigket von einem zum nächsten Segment im Mittel um einen Faktor von 2. Unsere experimentellen Daten waren die Grundlage für ein mathematisches Modell zur Beschreibung der Zellbewegung mit alternierender Geschwindigkeit. Die analytische Lösung des Modells zeigt elegant, dass eine Population von Bakterien, welche zwischen zwei Geschwindigkeiten wechseln, signifikant schneller expandiert als eine Referenzpopulation mit Bakterien konstanter Schwimmgeschwindkeit. Im Vergleich zu frei schwimmenden Bakterien beobachteten wir in der Nähe der Oberfläche eine um 15% erhöhte Schwimmgeschwindigkeit der Zellen und eine um 90 % erhöhte Winkel-geschwindigkeit. Außerdem wurde eine signifikant höhere Zelldichte in der Nähe der Grenzfläche gemessen. Während sich der Anstieg in der Winkelgeschwindigkeit durch ein Drehmoment erklären lässt, welches in Oberflächennähe auf den rotierenden Zellkörper und die rotierenden Flagellen wirkt, kann die Beschleunigung und Akkumulation der Zellen bei dem beobachteten Abstand nicht durch existierende Theorien erklärt werden. Unsere Ergebnisse lassen vermuten, dass neben hydrodynamischen Effekten auch Kollisionen mit der Oberfläche eine wichtige Rolle spielen und sich die Rotationsgeschwindigkeit der Flagellenmotoren in der Nähe einer festen Oberfläche grundsätzlich verändert. Unsere Experimente zum Zellwachstum an Oberflächen zeigten, dass sich etwa sechs Stunden nach Beginn des Experiments größere Kolonien an der Kanaloberfläche auflösen und Zellen für ca. 30 Minuten zurück in die schwimmende Phase wechseln. Ergebnisse von mehreren Vergleichsexperimenten deuten darauf hin, dass dieser Übergang nach einer festen Anzahl von Zellteilungen an der Oberfläche erfolgt und nicht durch den Verbrauch des Wachstumsmediums bedingt wird. KW - Pseudomonas putida KW - Motilität KW - Flagellenbewegung KW - Random-Walk-Theorie KW - Schwimmende Mikroorganismen KW - pseudomonas putida KW - motility KW - flagellar filaments KW - random walk KW - cell tracking Y1 - 2013 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-70313 ER - TY - THES A1 - Prokhorov, Boris E. T1 - High-latitude coupling processes between thermospheric circulation and solar wind driven magnetospheric currents and plasma convection T1 - Kopplungsprozesse zwischen der thermosphärischen Zirkulation in hohen Breiten und den vom Sonnenwind getriebenen magnetosphärischen Strömen und der Plasmakonvektion N2 - The high-latitudinal thermospheric processes driven by the solar wind and Interplanetary Magnetic Field (IMF) interaction with the Earth magnetosphere are highly variable parts of the complex dynamic plasma environment, which represent the coupled Magnetosphere – Ionosphere – Thermosphere (MIT) system. The solar wind and IMF interactions transfer energy to the MIT system via reconnection processes at the magnetopause. The Field Aligned Currents (FACs) constitute the energetic links between the magnetosphere and the Earth ionosphere. The MIT system depends on the highly variable solar wind conditions, in particular on changes of the strength and orientation of the IMF. In my thesis, I perform an investigation on the physical background of the complex MIT system using the global physical - numerical, three-dimensional, time-dependent and self-consistent Upper Atmosphere Model (UAM). This model describes the thermosphere, ionosphere, plasmasphere and inner magnetosphere as well as the electrodynamics of the coupled MIT system for the altitudinal range from 80 (60) km up to the 15 Earth radii. In the present study, I developed and investigated several variants of the high-latitudinal electrodynamic coupling by including the IMF dependence of FACs into the UAM model. For testing, the various variants were applied to simulations of the coupled MIT system for different seasons, geomagnetic activities, various solar wind and IMF conditions. Additionally, these variants of the theoretical model with the IMF dependence were compared with global empirical models. The modelling results for the most important thermospheric parameters like neutral wind and mass density were compared with satellite measurements. The variants of the UAM model with IMF dependence show a good agreement with the satellite observations. In comparison with the empirical models, the improved variants of the UAM model reproduce a more realistic meso-scale structures and dynamics of the coupled MIT system than the empirical models, in particular at high latitudes. The new configurations of the UAM model with IMF dependence contribute to the improvement of space weather prediction. N2 - Die thermosphärischen Prozesse in hohen Breiten, die durch die Wechselwirkung des Sonnenwinds und des Interplanetaren Magnetfeldes (IMF) mit der Erdmagnetosphäre getrieben werden, stellen sich als stark veränderliches Geschehen in der komplexen dynamischen Plasmaumgebung der Erde dar, die das gekoppelte System der Magnetosphäre, Ionosphäre und Thermosphäre (MIT) umfaßt. Die Einflüsse des Sonnenwindes und des IMF zeigen sich als Energieübertragung in das MIT System mittels Rekonnektionsprozessen an der Magnetopause. Feldliniengerichtete Ströme (FACs) repräsentieren die energetische Kopplung zwischen der Magnetosphäre und der Ionosphäre der Erde. Das MIT System wird bestimmt durch die stark veränderlichen Sonnenwindbedingungen, insbesondere von der Stärke und Richtung des IMF. In meiner Promotionsschrift untersuche ich die physikalischen Bedingungen des komplexen MIT System mit Hilfe eines globalen physikalisch-numerischen, dreidimensionalen, zeitabhängigen und selbstkonsistenten Modells, dem Upper Atmosphere Model (UAM). Das UAM beschreibt das Verhalten der Thermosphäre, Ionosphäre, Plasmasphäre und der inneren Magnetosphäre in einem Höhenbereich zwischen 80 (60) km und 15 Erdradien sowie die elektrodynamische Verkopplung des gesamten MIT Systems. In der vorliegenden Arbeit habe ich mehrere Varianten der elektrodynamischen Kopplung in hohen Breiten entwickelt und analysiert, die die FACs innerhalb des UAM in ihrer Abhängigkeit vom IMF darstellen. Für Testzwecke wurden diese Varianten auf eine Reihe von numerischen Simulationen des gekoppelten MIT Systems unter verschiedenen Bedingungen hinsichtlich Jahreszeit, geomagnetischer Aktivität, Sonnenwind- und IMF-Parametern angewandt. Darüberhinaus wurden diese Varianten des IMF-abhängigen theoretischen Modells entsprechenden globalen empirischen Modellen gegenübergestellt. Modellergebnisse wurden außerdem mit einigen wichtigen von Satelliten gemessenen Thermosphärenparametern, wie dem Neutralwind und der Massendichte verglichen. Die UAM Modelvarianten mit IMF-Abhängigkeit zeigen eine gute Übereinstimmung mit den Satellitenbeobachtungen. Im Vergleich mit empirischen Modellaussagen geben die UAM Modellvarianten ein genaueres Bild der mesoskaligen Strukturen und der Dynamik des gekoppelten MIT Systems wieder, insbesondere für die hohen Breiten. Die neuen UAM Konfigurationen mit IMF-Abhängigkeit tragen damit zu verbesserten Möglichkeiten in der Weltraumwettervorhersage bei. KW - upper atmosphere model KW - high-latitudinal thermosphere KW - magnetosphere-ionosphere-thermosphere coupling KW - solar wind and interplanetary magnetic field influence KW - field aligned currents KW - Upper Atmosphere Model (UAM) KW - Thermosphäre hoher Breiten KW - Kopplung zwischen Magnetosphäre, Ionosphäre und Thermosphäre KW - Einfluß des Sonnenwindes und des interplanetaren magnetischen Feldes KW - feldlinengerichtete Ströme Y1 - 2015 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-92353 ER - TY - THES A1 - Schröder, Henning T1 - Ultrafast electron dynamics in Fe(CO)5 and Cr(CO)6 T1 - Ultraschnelle Elektronendynamik in Fe(CO)5 und Cr(CO)6 N2 - In this thesis, the two prototype catalysts Fe(CO)₅ and Cr(CO)₆ are investigated with time-resolved photoelectron spectroscopy at a high harmonic setup. In both of these metal carbonyls, a UV photon can induce the dissociation of one or more ligands of the complex. The mechanism of the dissociation has been debated over the last decades. The electronic dynamics of the first dissociation occur on the femtosecond timescale. For the experiment, an existing high harmonic setup was moved to a new location, was extended, and characterized. The modified setup can induce dynamics in gas phase samples with photon energies of 1.55eV, 3.10eV, and 4.65eV. The valence electronic structure of the samples can be probed with photon energies between 20eV and 40eV. The temporal resolution is 111fs to 262fs, depending on the combination of the two photon energies. The electronically excited intermediates of the two complexes, as well as of the reaction product Fe(CO)₄, could be observed with photoelectron spectroscopy in the gas phase for the first time. However, photoelectron spectroscopy gives access only to the final ionic states. Corresponding calculations to simulate these spectra are still in development. The peak energies and their evolution in time with respect to the initiation pump pulse have been determined, these peaks have been assigned based on literature data. The spectra of the two complexes show clear differences. The dynamics have been interpreted with the assumption that the motion of peaks in the spectra relates to the movement of the wave packet in the multidimensional energy landscape. The results largely confirm existing models for the reaction pathways. In both metal carbonyls, this pathway involves a direct excitation of the wave packet to a metal-to-ligand charge transfer state and the subsequent crossing to a dissociative ligand field state. The coupling of the electronic dynamics to the nuclear dynamics could explain the slower dissociation in Fe(CO)₅ as compared to Cr(CO)₆. N2 - Diese Dissertation handelt von der Untersuchung der zwei Modell-Katalysatoren Fe(CO)₅ und Cr(CO)₆ mittels zeitaufgelöster Photoelektronen Spektroskopie an einem High Harmonic Setup. In beiden Metallcarbonyl kann die Dissoziation von einem, oder mehreren Liganden durch ein UV Photon ausgelöst werden. Der Dissoziation-Mechanismus wurde in den letzten Jahrzehnten diskutiert. Die Abspaltung des ersten Liganden und die damit verbundenen elektronischen Dynamiken finden auf Zeitskalen von Femtosekunden statt. Für die Durchführung dieses Experiments wurde ein bestehender High Harmonic Setup in ein neues Labor verlegt. Der Aufbau wurde erweitert und charakterisiert. Mit dem modifizierten Aufbau können nun Reaktionen in Gas-Phasen-Proben mit Photonenenergien von 1.55eV, 3.10eV und 4.65eV ausgelöst werden. Dabei kann die Valenz-Elektronen-Struktur mit Photonenenergien zwischen 20eV und 40eV untersucht werden. Die Zeitauflösung liegt im Bereich von 111fs bis 262fs und hängt von der Kombination der zwei Photonenenergien ab. Die beiden Komplexe sowie Fe(CO)₄ konnten in der Gas-Phase zum ersten Mal in elektronisch angeregten Zuständen mittels zeitaufgelöster Photoelektronenspektroskopie beobachtet werden. Im Allgemeinen kann jedoch mit der Photoelektronenspektroskopie nur der ionische Endzustand untersucht werden. Modellrechnungen zu den Spektren und die Entwicklung der dazugehörigen Theorie befinden derzeit noch in der Entwicklungsphase. Die Peaks in den Spektren konnten anhand von Literatur zugeordnet werden. Die Spektren der beiden Komplexe unterscheiden sich deutlich. Zu deren Interpretation wurde die Näherung verwendet, dass die Dynamik der Peaks in den Spektren die Bewegung des Wellenpakets in der multidimensionalen Energielandschaft darstellt. Die neuen Daten bestätigen weitestgehend bestehende Modelle für die Reaktionsmechanismen. Der Reaktionsmechanismus verläuft für beide Metallcarbonyle über eine direkte Anregung des Wellenpakets in einen metal-to-ligand charge transfer Zustand. Von dem angeregten Zustand aus kann das Wellenpaket in den dissoziativen ligand field Zustand wechseln. Dass die Reaktion in Fe(CO)₅ langsamer als in Cr(CO)₆ abläuft, kann durch die Kopplung der Dynamiken von Elektronen und Kernen erklärt werden. KW - dissertation KW - Dissertation KW - photo electron spectroscopy KW - physical chemistry KW - molecular dynamics KW - high harmonic generation KW - iron pentacarbonyl KW - chromium hexacarbonyl KW - metal carbonyls KW - ultrafast KW - dynamics KW - Photoelektronen KW - Spektroskopie KW - Moleküldynamik KW - high harmonic KW - Eisenpentacarbonyl KW - Chromhexacarbonyl KW - Photodissoziation KW - photodissociation KW - ligand KW - bond Y1 - 2016 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-94589 ER - TY - THES A1 - Rezanezhad, Vahid T1 - Inversion of the 2004 M6.0 Parkfield Earthquake Coseismic Offsets by Partition Model Y1 - 2016 ER -