TY - JOUR A1 - Andersson, Edvin K. W. A1 - Sångeland, Christofer A1 - Berggren, Elin A1 - Johansson, Fredrik O. L. A1 - Kühn, Danilo A1 - Lindblad, Andreas A1 - Mindemark, Jonas A1 - Hahlin, Maria T1 - Early-stage decomposition of solid polymer electrolytes in Li-metal batteries JF - Journal of materials chemistry : A, Materials for energy and sustainability N2 - Development of functional and stable solid polymer electrolytes (SPEs) for battery applications is an important step towards both safer batteries and for the realization of lithium-based or anode-less batteries. The interface between the lithium and the solid polymer electrolyte is one of the bottlenecks, where severe degradation is expected. Here, the stability of three different SPEs - poly(ethylene oxide) (PEO), poly(epsilon-caprolactone) (PCL) and poly(trimethylene carbonate) (PTMC) - together with lithium bis(trifluoromethanesulfonyl)imide (LiTFSI) salt, is investigated after they have been exposed to lithium metal under UHV conditions. Degradation compounds, e.g. Li-O-R, LiF and LixSyOz, are identified for all SPEs using soft X-ray photoelectron spectroscopy. A competing degradation between polymer and salt is identified in the outermost surface region (<7 nm), and is dependent on the polymer host. PTMC:LiTFSI shows the most severe decomposition of both polymer and salt followed by PCL:LiTFSI and PEO:LiTFSI. In addition, the movement of lithium species through the decomposed interface shows large variation depending on the polymer electrolyte system. Y1 - 2021 U6 - https://doi.org/10.1039/d1ta05015j SN - 2050-7488 SN - 2050-7496 VL - 9 IS - 39 SP - 22462 EP - 22471 PB - Royal Society of Chemistry CY - Cambridge ER - TY - JOUR A1 - Andrianov, Igor V. A1 - Klamroth, Tillmann A1 - Saalfrank, Peter A1 - Bovensiepen, U. A1 - Gahl, Cornelius A1 - Wolf, M. M. T1 - Quantum theoretical study of electron solvation dynamics in ice layers on a Cu(111) surface N2 - Recent experiments using time- and angle-resolved two-photon photoemission (2PPE) spectroscopy at metal/polar adsorbate interfaces succeeded in time-dependent analysis of the process of electron solvation. A fully quantum mechanical, two-dimensional simulation of this process, which explicitly includes laser excitation, is presented here, confirming the origin of characteristic features, such as the experimental observation of an apparently negative dispersion. The inference of the spatial extent of the localized electron states from the angular dependence of the 2PPE spectra has been found to be non-trivial and system-dependent. (C) 2005 American Institute of Physics Y1 - 2005 SN - 0021-9606 ER - TY - JOUR A1 - Andrianov, Ivan A1 - Saalfrank, Peter T1 - Theoretical study of vibration-phonon coupling of H adsorbed on a Si(100) surface N2 - In this paper a perturbation-theory study of vibrational lifetimes for the bending and stretching modes of hydrogen adsorbed on a Si(100) surface is presented. The hydrogen-silicon interaction is treated with a semiempirical bond-order potential. Calculations are performed for H-Si clusters of different sizes. The finite lifetime is due to vibration-phonon coupling, which is assumed to be linear or bilinear in the phonon and nonlinear in the H-Si stretching and bending modes. Lifetimes and vibrational transition rates are evaluated with one- and two-phonon processes taken into account. Temperature effects are also discussed. In agreement with the experiment and previous theoretical treatment it is found that the H-Si (upsilon(s)=1) stretching vibration decays on a nanosecond timescale, whereas for the H-Si (upsilon(b)=1) bending mode a picosecond decay is predicted. For higher-excited vibrations, simple scaling laws are found if the excitation energies are not too large. The relaxation mechanisms for the excited H-Si stretching and the H-Si bending modes are analyzed in detail. Y1 - 2006 UR - http://jcp.aip.org/ U6 - https://doi.org/10.1063/1.2161191 SN - 0021-9606 ER - TY - JOUR A1 - Angelova, Angelina A1 - Ionov, Radoslav A1 - Reiche, Jürgen A1 - Brehmer, Ludwig T1 - Head-to tail or head-to-head structure of Langmuir-Blodgett long chain ester multilayers? Y1 - 1994 ER - TY - JOUR A1 - Angelova, Angelina A1 - Penacorada, Florencio A1 - Stiller, Burkhard A1 - Zetzsche, Thomas A1 - Ionov, Radoslav A1 - Kamusewitz, Helmut A1 - Brehmer, Ludwig T1 - Wettability, surface morphology and stability of long chain ester multilayers obtained by different Langmuir- Blodgett deposition type Y1 - 1994 ER - TY - JOUR A1 - Angelova, Angelina A1 - Reiche, Jürgen A1 - Ionov, Radoslav A1 - Janietz, Dietmar A1 - Lemmetyinen, Helge A1 - Brehmer, Ludwig T1 - Control of the structure of Langmuir-Blodgett films of a discotic liquid crystalline compound via the subphase composition and the adjacent molecular environment N2 - Changes of the molecular arrangenemt that can be induced by means of the LB technique in the multilayers of a disc-shaped multialkynyl amphiphile are monitored by means of small angle X-ray diffraction. Studies of the monolayers at the air-water interface reveal "edge-on" orientation of the discs. Specific effects of the counter- ions (Na+, Cd²+, Pb²+, and Ba²+) and sub-solution pH on the monolayer collapse pressure, transfer efficiency and molecular order in the multilayers are found. A correlation between the monolayer properties and the ability for formation of periodic discotic structures in the presence of divalent counterions is established. The discotic molecules retain their "edge-on" arrangement in the highly compressed transferred films with slight irregular interdigtation of the flexible wings and inclination to the substrate normal. The tilt and the inter- digitation are reduced when the discotic monolayers are deposited in alternating LB films with barium arachidate spacer layers. Y1 - 1994 ER - TY - THES A1 - Anggraini, Ade T1 - The 26 May 2006 yogyakarta earthquake, aftershocks and interactions Y1 - 2013 CY - Potsdam ER - TY - THES A1 - Anguiano, Borja T1 - The age-metallicity-velocity relation in the nearby disk Y1 - 2012 CY - Potsdam 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 - THES A1 - Anielski, Alexander T1 - Entwicklung einer mikrofluidischen, adaptiv geregelten Messapparatur zur quantitativen Untersuchung von Chemotaxis mit Hilfe der Flussfotolyse KW - Flussfotolyse KW - Konzentration KW - Chemotaxis KW - Mikrokanal KW - Dictyostelium KW - flow photolysis KW - concentration KW - chemotaxis KW - microchannel KW - Dictyostelium Y1 - 2015 ER - TY - JOUR A1 - Anielski, Alexander A1 - Barbosa Pfannes, Eva Katharina A1 - Beta, Carsten T1 - Adaptive microfluidic gradient generator for quantitative chemotaxis experiments JF - Review of scientific instruments : a monthly journal devoted to scientific instruments, apparatus, and techniques N2 - Chemotactic motion in a chemical gradient is an essential cellular function that controls many processes in the living world. For a better understanding and more detailed modelling of the underlying mechanisms of chemotaxis, quantitative investigations in controlled environments are needed. We developed a setup that allows us to separately address the dependencies of the chemotactic motion on the average background concentration and on the gradient steepness of the chemoattractant. In particular, both the background concentration and the gradient steepness can be kept constant at the position of the cell while it moves along in the gradient direction. This is achieved by generating a well-defined chemoattractant gradient using flow photolysis. In this approach, the chemoattractant is released by a light-induced reaction from a caged precursor in a microfluidic flow chamber upstream of the cell. The flow photolysis approach is combined with an automated real-time cell tracker that determines changes in the cell position and triggers movement of the microscope stage such that the cell motion is compensated and the cell remains at the same position in the gradient profile. The gradient profile can be either determined experimentally using a caged fluorescent dye or may be alternatively determined by numerical solutions of the corresponding physical model. To demonstrate the function of this adaptive microfluidic gradient generator, we compare the chemotactic motion of Dictyostelium discoideum cells in a static gradient and in a gradient that adapts to the position of the moving cell. Published by AIP Publishing. Y1 - 2017 U6 - https://doi.org/10.1063/1.4978535 SN - 0034-6748 SN - 1089-7623 VL - 88 PB - American Institute of Physics CY - Melville ER - TY - JOUR A1 - Anishchenko, Vadim S. A1 - Kopeikin, A. S. A1 - Kurths, Jürgen T1 - Studying hyperbolicity in chaotic systems Y1 - 2000 ER - TY - JOUR A1 - Anishchenko, Vadim S. A1 - Kopeikin, A. S. A1 - Vadivasova, T. E. T1 - Influence of noise on statistical properties of nonhyperbolic attractors Y1 - 2000 ER - TY - JOUR A1 - Anishchenko, Vadim S. A1 - Nikolaev, S A1 - Kurths, Jürgen T1 - Winding number locking on a two-dimensional torus : synchronization of quasiperiodic motions N2 - We propose a new autonomous dynamical system of dimension N=4 that demonstrates the regime of stable two- frequency motions and period-doubling bifurcations of a two-dimensional torus. It is shown that the period-doubling bifurcation of the two-dimensional torus is not followed by the resonance phenomenon, and the two-dimensional ergodic torus undergoes a period-doubling bifurcation. The interaction of two generators is also analyzed. The phenomenon of external and mutual synchronization of two-frequency oscillations is observed, for which winding number locking on a two- dimensional torus takes place Y1 - 2006 UR - http://pre.aps.org/ U6 - https://doi.org/10.1103/Physreve.73.056202 SN - 1539-3755 ER - TY - JOUR A1 - Anishchenko, Vadim S. A1 - Vadivasova, T. E. A1 - Kopeikin, A. S. A1 - Kurths, Jürgen A1 - Strelkova, G. I. T1 - Effect of noise on the relaxation to an invariant probability measure of nonhyperbolic chaotic attractors Y1 - 2001 ER - TY - JOUR A1 - Anishchenko, Vadim S. A1 - Vadivasova, T. E. A1 - Kopeikin, A. S. A1 - Strelkova, G. I. A1 - Kurths, Jürgen T1 - Spectral and correlation analysis of spiral chaos N2 - We study numerically the behavior of the autocorrelation function (ACF) and the power spectrum of spiral attractors without and in the presence of noise. It is shown that the ACF decays exponentially and has two different time scales. The rate of the ACF decrease is defined by the amplitude fluctuations on small time intervals, i.e., when tau < tau(cor), and by the effective diffusion coefficient of the instantantaneous phase on large time intervals. it is also demonstrated that the ACF in the Poincare map also decreases according to the exponential law exp(-lambda(+)k), where lambda(+) is the positive Lyapunov exponent. The obtained results are compared with the theory of fluctuations for the Van der Pol oscillator Y1 - 2003 SN - 0219-4775 ER - TY - JOUR A1 - Anishchenko, Vadim S. A1 - Vadivasova, T. E. A1 - Kurths, Jürgen A1 - Okrokvertskhov, G. A. A1 - Strelkova, G. I. T1 - Autocorrelation function and spectral linewidth of spiral chaos in a physical experiment N2 - We present results of physical experiments where we measure the autocorrelation function (ACF) and the spectral linewidth of the basic frequency of a spiral chaotic attractor in a generator with inertial nonlinearity both without and in the presence of external noise. It is shown that the ACF of spiral attractors decays according to an exponential law with a decrement which is defined by the phase diffusion coefficient. It is also established that the evolution of the instantaneous phase can be approximated by a Wiener random process Y1 - 2004 SN - 1063-651X ER - TY - JOUR A1 - Anton, Arthur Markus A1 - Steyrleuthner, Robert A1 - Kossack, Wilhelm A1 - Neher, Dieter A1 - Kremer, Friedrich T1 - Infrared Transition Moment Orientational Analysis on the Structural Organization of the Distinct Molecular Subunits in Thin Layers of a High Mobility n-Type Copolymer JF - Journal of the American Chemical Society N2 - The IR-based method of infrared transition moment orientational analysis (IR-TMOA) is employed to unravel molecular order in thin layers of the semiconducting polymer poly[N,N'-bis(2-octyldodecyl),-1,4,5,8-naphthalene-diimide-2,6-diyl]-alt-5-5'-(2,2'-bithiophene) (P(NDI2OD-T2)). Structure-specific vibrational bands are analyzed in dependence On polarization and inclination of the sample-With respect to the optical axis. By that the molecular Order parameter tensor for the respective molecular moieties with regard to the sample: coordinate system is deduced. Making use of the specificity of the IR spectral range, we are able to determine separately the orientation of atomistic planes defined through the naphthalenediimide (NDI) and bithiophene (T2) units relative to the substrate, and hence, relative to each other. A pronounced solvent effect is observed While chlorobenzene causes the T2 planes to align preferentially parallel to the substrate at an angle of 29 degrees, using a 1:1 chloronaphthalene:xylene mixture results in a reorientation of the T2 units from a face on into an edge on arrangement. In contrast the NDI unit remains unaffected. Additionally, for both solvents evidence is observed for the aggregation of chains in accord With recently published results obtained by UV-vis absorption spectroscopy. Y1 - 2015 U6 - https://doi.org/10.1021/jacs.5b01755 SN - 0002-7863 VL - 137 IS - 18 SP - 6034 EP - 6043 PB - American Chemical Society CY - Washington ER - TY - THES A1 - Antonelli, Andrea T1 - Accurate waveform models for gravitational-wave astrophysics: synergetic approaches from analytical relativity N2 - Gravitational-wave (GW) astrophysics is a field in full blossom. Since the landmark detection of GWs from a binary black hole on September 14th 2015, fifty-two compact-object binaries have been reported by the LIGO-Virgo collaboration. Such events carry astrophysical and cosmological information ranging from an understanding of how black holes and neutron stars are formed, what neutron stars are composed of, how the Universe expands, and allow testing general relativity in the highly-dynamical strong-field regime. It is the goal of GW astrophysics to extract such information as accurately as possible. Yet, this is only possible if the tools and technology used to detect and analyze GWs are advanced enough. A key aspect of GW searches are waveform models, which encapsulate our best predictions for the gravitational radiation under a certain set of parameters, and that need to be cross-correlated with data to extract GW signals. Waveforms must be very accurate to avoid missing important physics in the data, which might be the key to answer the fundamental questions of GW astrophysics. The continuous improvements of the current LIGO-Virgo detectors, the development of next-generation ground-based detectors such as the Einstein Telescope or the Cosmic Explorer, as well as the development of the Laser Interferometer Space Antenna (LISA), demand accurate waveform models. While available models are enough to capture the low spins, comparable-mass binaries routinely detected in LIGO-Virgo searches, those for sources from both current and next-generation ground-based and spaceborne detectors must be accurate enough to detect binaries with large spins and asymmetry in the masses. Moreover, the thousands of sources that we expect to detect with future detectors demand accurate waveforms to mitigate biases in the estimation of signals’ parameters due to the presence of a foreground of many sources that overlap in the frequency band. This is recognized as one of the biggest challenges for the analysis of future-detectors’ data, since biases might hinder the extraction of important astrophysical and cosmological information from future detectors’ data. In the first part of this thesis, we discuss how to improve waveform models for binaries with high spins and asymmetry in the masses. In the second, we present the first generic metrics that have been proposed to predict biases in the presence of a foreground of many overlapping signals in GW data. For the first task, we will focus on several classes of analytical techniques. Current models for LIGO and Virgo studies are based on the post-Newtonian (PN, weak-field, small velocities) approximation that is most natural for the bound orbits that are routinely detected in GW searches. However, two other approximations have risen in prominence, the post-Minkowskian (PM, weak- field only) approximation natural for unbound (scattering) orbits and the small-mass-ratio (SMR) approximation typical of binaries in which the mass of one body is much bigger than the other. These are most appropriate to binaries with high asymmetry in the masses that challenge current waveform models. Moreover, they allow one to “cover” regions of the parameter space of coalescing binaries, thereby improving the interpolation (and faithfulness) of waveform models. The analytical approximations to the relativistic two-body problem can synergically be included within the effective-one-body (EOB) formalism, in which the two-body information from each approximation can be recast into an effective problem of a mass orbiting a deformed Schwarzschild (or Kerr) black hole. The hope is that the resultant models can cover both the low-spin comparable-mass binaries that are routinely detected, and the ones that challenge current models. The first part of this thesis is dedicated to a study about how to best incorporate information from the PN, PM, SMR and EOB approaches in a synergistic way. We also discuss how accurate the resulting waveforms are, as compared against numerical-relativity (NR) simulations. We begin by comparing PM models, whether alone or recast in the EOB framework, against PN models and NR simulations. We will show that PM information has the potential to improve currently-employed models for LIGO and Virgo, especially if recast within the EOB formalism. This is very important, as the PM approximation comes with a host of new computational techniques from particle physics to exploit. Then, we show how a combination of PM and SMR approximations can be employed to access previously-unknown PN orders, deriving the third subleading PN dynamics for spin-orbit and (aligned) spin1-spin2 couplings. Such new results can then be included in the EOB models currently used in GW searches and parameter estimation studies, thereby improving them when the binaries have high spins. Finally, we build an EOB model for quasi-circular nonspinning binaries based on the SMR approximation (rather than the PN one as usually done). We show how this is done in detail without incurring in the divergences that had affected previous attempts, and compare the resultant model against NR simulations. We find that the SMR approximation is an excellent approximation for all (quasi-circular nonspinning) binaries, including both the equal-mass binaries that are routinely detected in GW searches and the ones with highly asymmetric masses. In particular, the SMR-based models compare much better than the PN models, suggesting that SMR-informed EOB models might be the key to model binaries in the future. In the second task of this thesis, we work within the linear-signal ap- proximation and describe generic metrics to predict inference biases on the parameters of a GW source of interest in the presence of confusion noise from unfitted foregrounds and from residuals of other signals that have been incorrectly fitted out. We illustrate the formalism with simple (yet realistic) LISA sources, and demonstrate its validity against Monte-Carlo simulations. The metrics we describe pave the way for more realistic studies to quantify the biases with future ground-based and spaceborne detectors. N2 - Wenn zwei kompakte Objekte wie Schwarze Löcher oder Neutronensterne kollidieren, wird der Raum und die Zeit um sie herum stark gekrümmt. Der effekt sind Störungen der Raumzeit, sogenannte Gravitationswellen, die sich im gesamten Universum ausbreiten. Mit den leistungsstarken und präzisen Netzwerken von Detektoren und der Arbeit vieler Wissenschaftler rund um den Globus kann man Gravitationswellen auf der Erde messen. Gravitationswellen tragen Informationen über das System, das sie erzeugt hat. Insbesondere kann man erfahren, wie sich die kompakten Objekte gebildet haben und woraus sie bestehen. Daraus lässt sich ableiten, wie sich das Universum ausdehnt, und man kann die Allgemeine Relativitätstheorie in Regionen mit starker Gravitation testen. Um diese Informationen zu extrahieren, werden genaue Modelle benötigt. Modelle können entweder numerisch durch Lösen der berühmten Einstein-Gleichungen oder analytisch durch Annäherung an deren Lösungen gewonnen werden. In meiner Arbeit haben wir den zweiten Ansatz verfolgt, um sehr genaue Vorhersagen für die Signale zu erhalten, die bei kommenden Beobachtungen durch Gravitationswellendetektoren verwendet werden können. KW - gravitational waves KW - Gravitationswellen KW - general relativity KW - allgemeine Relativitätstheorie KW - data analysis KW - Datenanalyse Y1 - 2021 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-576671 ER - TY - THES A1 - Aranda Espinoza, Said Eduardo T1 - Deformation of model membranes subjected to alternating electric fields Y1 - 2008 ER - TY - JOUR A1 - Aranson, Igor S. A1 - Pikovskij, Arkadij T1 - Confinement and collective escape of active particles JF - Physical review letters N2 - Active matter broadly covers the dynamics of self-propelled particles. While the onset of collective behavior in homogenous active systems is relatively well understood, the effect of inhomogeneities such as obstacles and traps lacks overall clarity. Here, we study how interacting, self-propelled particles become trapped and released from a trap. We have found that captured particles aggregate into an orbiting condensate with a crystalline structure. As more particles are added, the trapped condensates escape as a whole. Our results shed light on the effects of confinement and quenched disorder in active matter. Y1 - 2022 U6 - https://doi.org/10.1103/PhysRevLett.128.108001 SN - 0031-9007 SN - 1079-7114 SN - 1092-0145 VL - 128 IS - 10 PB - American Physical Society CY - College Park, Md. ER - TY - THES A1 - Arbabi-Bidgoli, Sepehr T1 - Voids in the Large Scale Structure of the Universe Y1 - 2003 ER - TY - JOUR A1 - Archambault, S. A1 - Archer, A. A1 - Aune, T. A1 - Barnacka, Anna A1 - Benbow, W. A1 - Bird, R. A1 - Buchovecky, M. A1 - Buckley, J. H. A1 - Bugaev, V. A1 - Byrum, K. A1 - Cardenzana, J. V. A1 - Cerruti, M. A1 - Chen, Xuhui A1 - Ciupik, L. A1 - Collins-Hughes, E. A1 - Connolly, M. P. A1 - Cui, W. A1 - Dickinson, H. J. A1 - Dumm, J. A1 - Eisch, J. D. A1 - Falcone, A. A1 - Feng, Q. A1 - Finley, J. P. A1 - Fleischhack, H. A1 - Flinders, A. A1 - Fortin, P. A1 - Fortson, L. A1 - Furniss, A. A1 - Gillanders, G. H. A1 - Griffin, S. A1 - Grube, J. A1 - Gyuk, G. A1 - Huetten, M. A1 - Hakansson, Nils A1 - Hanna, D. A1 - Holder, J. A1 - Humensky, T. B. A1 - Johnson, C. A. A1 - Kaaret, P. A1 - Kar, P. A1 - Kelley-Hoskins, N. A1 - Kertzman, M. A1 - Khassen, Y. A1 - Kieda, D. A1 - Krause, M. A1 - Krennrich, F. A1 - Kumar, S. A1 - Lang, M. J. A1 - Maier, G. A1 - McArthur, S. A1 - McCann, A. A1 - Meagher, K. A1 - Millis, J. A1 - Moriarty, P. A1 - Mukherjee, R. A1 - Nieto, D. A1 - Ong, R. A. A1 - Otte, A. N. A1 - Pandel, D. A1 - Park, N. A1 - Pelassa, V. A1 - Pohl, Martin A1 - Popkow, A. A1 - Pueschel, Elisa A1 - Quinn, J. A1 - Ragan, K. A1 - Reynolds, P. T. A1 - Richards, G. T. A1 - Roache, E. A1 - Rousselle, J. A1 - Rulten, C. A1 - Santander, M. A1 - Sembroski, G. H. A1 - Shahinyan, K. A1 - Smith, A. W. A1 - Staszak, D. A1 - Telezhinsky, Igor O. A1 - Tucci, J. V. A1 - Tyler, J. A1 - Vincent, S. A1 - Wakely, S. P. A1 - Weiner, O. M. A1 - Weinstein, A. A1 - Wilhelm, Alina A1 - Williams, D. A. A1 - Zitzer, B. T1 - EXCEPTIONALLY BRIGHT TEV FLARES FROM THE BINARY LS I+61 degrees 303 JF - The astrophysical journal : an international review of spectroscopy and astronomical physics ; Part 2, Letters N2 - The TeV binary system LS I +61 degrees 303 is known for its regular, non-thermal emission pattern that traces the orbital period of the compact object in its 26.5 day orbit around its B0 Ve star companion. The system typically presents elevated TeV emission around apastron passage with flux levels between 5% and 15% of the steady flux from the Crab Nebula (> 300 GeV). In this article, VERITAS observations of LS I + 61 degrees. 303 taken in late 2014 are presented, during which bright TeV flares around apastron at flux levels peaking above 30% of the Crab Nebula flux were detected. This is the brightest such activity from this source ever seen in the TeV regime. The strong outbursts have rise and fall times of less than a day. The short timescale of the flares, in conjunction with the observation of 10 TeV photons from LS I + 61 degrees 303 during the flares, provides constraints on the properties of the accelerator in the source. KW - binaries: general KW - gamma-rays: general KW - stars: individual (LS I+61 degrees 303, VER J0240+612) KW - X-rays: binaries Y1 - 2016 U6 - https://doi.org/10.3847/2041-8205/817/1/L7 SN - 2041-8205 SN - 2041-8213 VL - 817 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Archambault, S. A1 - Archer, A. A1 - Barnacka, Anna A1 - Behera, B. A1 - Beilicke, M. A1 - Benbow, W. A1 - Berger, K. A1 - Bird, R. A1 - Böttcher, Markus A1 - Buckley, J. H. A1 - Bugaev, V. A1 - Cardenzana, J. V. A1 - Cerruti, M. A1 - Chen, Xuhui A1 - Christiansen, J. L. A1 - Ciupik, L. A1 - Collins-Hughes, E. A1 - Connolly, M. P. A1 - Cui, W. A1 - Dickinson, H. J. A1 - Dumm, J. A1 - Eisch, J. D. A1 - Errando, M. A1 - Falcone, A. A1 - Federici, Simone A1 - Feng, Q. A1 - Finley, J. P. A1 - Fleischhack, H. A1 - Fortson, L. A1 - Furniss, A. A1 - Gillanders, G. H. A1 - Godambe, S. A1 - Griffin, S. A1 - Griffiths, S. T. A1 - Grube, J. A1 - Gyuk, G. A1 - Hakansson, Nils A1 - Hanna, D. A1 - Holder, J. A1 - Hughes, G. A1 - Johnson, C. A. A1 - Kaaret, P. A1 - Kar, P. A1 - Kertzman, M. A1 - Khassen, Y. A1 - Kieda, D. A1 - Krawczynski, H. A1 - Kumar, S. A1 - Lang, M. J. A1 - Madhavan, A. S. A1 - Maier, G. A1 - McArthur, S. A1 - McCann, A. A1 - Meagher, K. A1 - Millis, J. A1 - Moriarty, P. A1 - Nelson, T. A1 - Nieto, D. A1 - Ong, R. A. A1 - Otte, A. N. A1 - Park, N. A1 - Perkins, J. S. A1 - Pohl, Martin A1 - Popkow, A. A1 - Prokoph, H. A1 - Pueschel, Elisa A1 - Quinn, J. A1 - Ragan, K. A1 - Rajotte, J. A1 - Reyes, L. C. A1 - Reynolds, P. T. A1 - Richards, G. T. A1 - Roache, E. A1 - Sembroski, G. H. A1 - Shahinyan, K. A1 - Smith, A. W. A1 - Staszak, D. A1 - Sweeney, K. A1 - Telezhinsky, Igor O. A1 - Tucci, J. V. A1 - Tyler, J. A1 - Varlotta, A. A1 - Vassiliev, V. V. A1 - Wakely, S. P. A1 - Welsing, R. A1 - Wilhelm, Alina A1 - Williams, D. A. A1 - Zitzer, B. T1 - Discovery of very high energy gamma rays from 1ES 1440+122 JF - Monthly notices of the Royal Astronomical Society KW - BL Lacertae objects: general KW - gamma-rays: general Y1 - 2016 U6 - https://doi.org/10.1093/mnras/stw1319 SN - 0035-8711 SN - 1365-2966 VL - 461 SP - 202 EP - 208 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Archambault, S. A1 - Archer, A. A1 - Benbow, W. A1 - Bird, R. A1 - Biteau, Jonathan A1 - Buchovecky, M. A1 - Buckley, J. H. A1 - Bugaev, V. A1 - Byrum, K. A1 - Cerruti, M. A1 - Chen, Xuhui A1 - Ciupik, L. A1 - Connolly, M. P. A1 - Cui, W. A1 - Eisch, J. D. A1 - Errando, M. A1 - Falcone, A. A1 - Feng, Q. A1 - Finley, J. P. A1 - Fleischhack, H. A1 - Fortin, P. A1 - Fortson, L. A1 - Furniss, A. A1 - Gillanders, G. H. A1 - Griffin, S. A1 - Grube, J. A1 - Gyuk, G. A1 - Huetten, M. A1 - Hakansson, Nils A1 - Hanna, D. A1 - Holder, J. A1 - Humensky, T. B. A1 - Johnson, C. A. A1 - Kaaret, P. A1 - Kar, P. A1 - Kelley-Hoskins, N. A1 - Kertzman, M. A1 - Kieda, D. A1 - Krause, M. A1 - Krennrich, F. A1 - Kumar, S. A1 - Lang, M. J. A1 - Maier, G. A1 - McArthur, S. A1 - McCann, A. A1 - Meagher, K. A1 - Moriarty, P. A1 - Mukherjee, R. A1 - Nguyen, T. A1 - Nieto, D. A1 - Ong, R. A. A1 - Otte, A. N. A1 - Park, N. A1 - Perkins, J. S. A1 - Pichel, A. A1 - Pohl, Martin A1 - Popkow, A. A1 - Pueschel, Elisa A1 - Quinn, J. A1 - Ragan, K. A1 - Reynolds, P. T. A1 - Richards, G. T. A1 - Roache, E. A1 - Rovero, A. C. A1 - Santander, M. A1 - Sembroski, G. H. A1 - Shahinyan, K. A1 - Smith, A. W. A1 - Staszak, D. A1 - Telezhinsky, Igor O. A1 - Tucci, J. V. A1 - Tyler, J. A1 - Vincent, S. A1 - Wakely, S. P. A1 - Weiner, O. M. A1 - Weinstein, A. A1 - Williams, D. A. A1 - Zitzer, B. A1 - Fumagalli, M. A1 - Prochaska, J. X. T1 - UPPER LIMITS FROM FIVE YEARS OF BLAZAR OBSERVATIONS WITH THE VERITAS CHERENKOV TELESCOPES JF - The astronomical journal N2 - Between the beginning of its full-scale scientific operations in 2007 and 2012, the VERITAS Cherenkov telescope array observed more than 130 blazars; of these, 26 were detected as very-high-energy (VHE; E > 100 GeV) gamma-ray sources. In this work, we present the analysis results of a sample of 114 undetected objects. The observations constitute a total live-time of similar to 570 hr. The sample includes several unidentified Fermi-Large Area Telescope (LAT) sources (located at high Galactic latitude) as well as all the sources from the second Fermi-LAT catalog that are contained within the field of view of the VERITAS observations. We have also performed optical spectroscopy measurements in order to estimate the redshift of some of these blazars that do not have spectroscopic distance estimates. We present new optical spectra from the Kast instrument on the Shane telescope at the Lick observatory for 18 blazars included in this work, which allowed for the successful measurement or constraint on the redshift of four of them. For each of the blazars included in our sample, we provide the flux upper limit in the VERITAS energy band. We also study the properties of the significance distributions and we present the result of a stacked analysis of the data set, which shows a 4s excess. KW - BL Lacertae objects: general KW - galaxies: active KW - gamma rays: galaxies KW - radiation mechanisms: non-thermal Y1 - 2016 U6 - https://doi.org/10.3847/0004-6256/151/6/142 SN - 0004-6256 SN - 1538-3881 VL - 151 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Archambault, S. A1 - Archer, A. A1 - Benbow, W. A1 - Bird, R. A1 - Bourbeau, E. A1 - Brantseg, T. A1 - Buchovecky, M. A1 - Buckley, J. H. A1 - Bugaev, V. A1 - Byrum, K. A1 - Cerruti, M. A1 - Christiansen, J. L. A1 - Connolly, M. P. A1 - Cui, W. A1 - Daniel, M. K. A1 - Feng, Q. A1 - Finley, J. P. A1 - Fleischhack, H. A1 - Fortson, L. A1 - Furniss, A. A1 - Geringer-Sameth, A. A1 - Griffin, S. A1 - Grube, J. A1 - Hütten, M. A1 - Hakansson, N. A1 - Hanna, D. A1 - Hervet, O. A1 - Holder, J. A1 - Hughes, G. A1 - Hummensky, B. A1 - Johnson, C. A. A1 - Kaaret, P. A1 - Kar, P. A1 - Kelley-Hoskins, N. A1 - Kertzman, M. A1 - Kieda, D. A1 - Koushiappas, S. A1 - Krause, M. A1 - Krennrich, F. A1 - Lang, M. J. A1 - Lin, T. T. Y. A1 - McArthur, S. A1 - Moriarty, P. A1 - Mukherjee, R. A1 - Nieto, D. A1 - Ong, R. A. A1 - Otte, A. N. A1 - Park, N. A1 - Pohl, M. A1 - Popkow, A. A1 - Pueschel, Elisa A1 - Quinn, J. A1 - Ragan, K. A1 - Reynolds, P. T. A1 - Richards, G. T. A1 - Roache, E. A1 - Rulten, C. A1 - Sadeh, I. A1 - Santander, M. A1 - Sembroski, G. H. A1 - Shahinyan, K. A1 - Smith, A. W. A1 - Staszak, D. A1 - Telezhinsky, Igor O. A1 - Trepanier, S. A1 - Tucci, J. V. A1 - Tyler, J. A1 - Wakely, S. P. A1 - Weinstein, A. A1 - Wilcox, P. A1 - Williams, D. A. A1 - Zitzer, B. T1 - Dark matter constraints from a joint analysis of dwarf Spheroidal galaxy observations with VERITAS JF - Physical review : D, Particles, fields, gravitation, and cosmology N2 - We present constraints on the annihilation cross section of weakly interacting massive particles dark matter based on the joint statistical analysis of four dwarf galaxies with VERITAS. These results are derived from an optimized photon weighting statistical technique that improves on standard imaging atmospheric Cherenkov telescope (IACT) analyses by utilizing the spectral and spatial properties of individual photon events. We report on the results of similar to 230 hours of observations of five dwarf galaxies and the joint statistical analysis of four of the dwarf galaxies. We find no evidence of gamma-ray emission from any individual dwarf nor in the joint analysis. The derived upper limit on the dark matter annihilation cross section from the joint analysis is 1.35 x 10(-23) cm(3) s(-1) at 1 TeV for the bottom quark (b (b) over bar) final state, 2.85 x 10(-24) cm(3) s(-1) at 1 TeV for the tau lepton (tau+tau(-)) final state and 1.32 x 10-25 cm(3) s(-1) at 1 TeV for the gauge boson (gamma gamma) final state. Y1 - 2017 U6 - https://doi.org/10.1103/PhysRevD.95.082001 SN - 2470-0010 SN - 2470-0029 VL - 95 IS - 8 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Archambault, S. A1 - Archer, A. A1 - Benbow, W. A1 - Bird, Ralph A1 - Bourbeau, E. A1 - Bouvier, A. A1 - Buchovecky, M. A1 - Bugaev, V. A1 - Cardenzana, J. V. A1 - Cerruti, M. A1 - Ciupik, L. A1 - Connolly, M. P. A1 - Cui, W. A1 - Daniel, M. K. A1 - Errando, M. A1 - Falcone, A. A1 - Feng, Q. A1 - Finley, J. P. A1 - Fleischhack, H. A1 - Fortson, L. A1 - Furniss, A. A1 - Gillanders, G. H. A1 - Griffin, S. A1 - Hanna, D. A1 - Hervet, O. A1 - Holder, J. A1 - Hughes, G. A1 - Humensky, T. B. A1 - Hutten, M. A1 - Johnson, C. A. A1 - Kaaret, P. A1 - Kar, P. A1 - Kertzman, M. A1 - Kieda, D. A1 - Krause, M. A1 - Lang, M. J. A1 - Lin, T. T. Y. A1 - Maier, G. A1 - McArthur, S. A1 - Moriarty, P. A1 - Mukherjee, R. A1 - Nieto, D. A1 - Ong, R. A. A1 - Otte, A. N. A1 - Park, N. A1 - Pohl, Martin A1 - Popkow, A. A1 - Pueschel, Elisa A1 - Quinn, J. A1 - Ragan, K. A1 - Reynolds, P. T. A1 - Richards, G. T. A1 - Roache, E. A1 - Rulten, C. A1 - Sadeh, I. A1 - Sembroski, G. H. A1 - Shahinyan, K. A1 - Staszak, D. A1 - Telezhinsky, Igor O. A1 - Trepanier, S. A1 - Wakely, S. P. A1 - Weinstein, A. A1 - Wilcox, P. A1 - Williams, D. A. A1 - Zitzer, B. T1 - Gamma-ray observations under bright moonlight with VERITAS JF - Astroparticle physics N2 - Imaging atmospheric Cherenkov telescopes (IACTs) are equipped with sensitive photomultiplier tube (PMT) cameras. Exposure to high levels of background illumination degrades the efficiency of and potentially destroys these photo-detectors over time, so IACTs cannot be operated in the same configuration in the presence of bright moonlight as under dark skies. Since September 2012, observations have been carried out with the VERITAS IACTs under bright moonlight (defined as about three times the night-sky-background (NSB) of a dark extragalactic field, typically occurring when Moon illumination > 35%) in two observing modes, firstly by reducing the voltage applied to the PMTs and, secondly, with the addition of ultra-violet (UV) bandpass filters to the cameras. This has allowed observations at up to about 30 times previous NSB levels (around 80% Moon illumination), resulting in 30% more observing time between the two modes over the course of a year. These additional observations have already allowed for the detection of a flare from the 1ES 1727 + 502 and for an observing program targeting a measurement of the cosmic-ray positron fraction. We provide details of these new observing modes and their performance relative to the standard VERITAS observations. (C) 2017 Elsevier B.V. All rights reserved. KW - Instrumentation KW - Moonlight KW - Observing methods KW - VERITAS KW - IACT Y1 - 2017 U6 - https://doi.org/10.1016/j.astropartphys.2017.03.001 SN - 0927-6505 SN - 1873-2852 VL - 91 SP - 34 EP - 43 PB - Elsevier CY - Amsterdam ER - TY - JOUR A1 - Archambault, S. A1 - Archer, A. A1 - Benbow, W. A1 - Buchovecky, M. A1 - Bugaev, V. A1 - Cerruti, M. A1 - Connolly, M. P. A1 - Cui, W. A1 - Falcone, A. A1 - Alonso, M. Fernandez A1 - Finley, J. P. A1 - Fleischhack, H. A1 - Fortson, L. A1 - Furniss, A. A1 - Griffin, S. A1 - Hutten, M. A1 - Hervet, O. A1 - Holder, J. A1 - Humensky, T. B. A1 - Johnson, C. A. A1 - Kaaret, P. A1 - Kar, P. A1 - Kieda, D. A1 - Krause, M. A1 - Krennrich, F. A1 - Lang, M. J. A1 - Lin, T. T. Y. A1 - Maier, G. A1 - McArthur, S. A1 - Moriarty, P. A1 - Nieto, D. A1 - Ong, R. A. A1 - Otte, A. N. A1 - Pohl, M. A1 - Popkow, A. A1 - Pueschel, Elisa A1 - Quinn, J. A1 - Ragan, K. A1 - Reynolds, P. T. A1 - Richards, G. T. A1 - Roache, E. A1 - Rovero, A. C. A1 - Sadeh, I. A1 - Shahinyan, K. A1 - Staszak, D. A1 - Telezhinsky, Igor O. A1 - Tyler, J. A1 - Wakely, S. P. A1 - Weinstein, A. A1 - Weisgarber, T. A1 - Wilcox, P. A1 - Wilhelm, Alina A1 - Williams, D. A. A1 - Zitzer, B. T1 - Search for Magnetically Broadened Cascade Emission from Blazars with VERITAS JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - We present a search for magnetically broadened gamma-ray emission around active galactic nuclei (AGNs), using VERITAS observations of seven hard-spectrum blazars. A cascade process occurs when multi-TeV gamma-rays from an AGN interact with extragalactic background light (EBL) photons to produce electron-positron pairs, which then interact with cosmic microwave background photons via inverse-Compton scattering to produce gamma-rays. Due to the deflection of the electron- positron pairs, a non-zero intergalactic magnetic field (IGMF) would potentially produce detectable effects on the angular distribution of the cascade emission. In particular, an angular broadening compared to the unscattered emission could occur. Through non-detection of angularly broadened emission from 1ES 1218 vertical bar 304, the source with the largest predicted cascade fraction, we exclude a range of IGMF strengths around 10(-14) G at the 95% confidence level. The extent of the exclusion range varies with the assumptions made about the intrinsic spectrum of 1ES. 1218+304 and the EBL model used in the simulation of the cascade process. All of the sources are used to set limits on the flux due to extended emission. KW - BL Lacertae objects: general KW - galaxies: active KW - gamma rays: galaxies KW - magnetic fields Y1 - 2017 U6 - https://doi.org/10.3847/1538-4357/835/2/288 SN - 0004-637X SN - 1538-4357 VL - 835 IS - 2 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Archambault, S. A1 - Archer, A. A1 - Benbow, Wystan A1 - Bird, Ralph A1 - Bourbeau, E. A1 - Buchovecky, M. A1 - Buckley, J. H. A1 - Bugaev, V. A1 - Cerruti, M. A1 - Connolly, M. P. A1 - Cui, W. A1 - Dwarkadas, Vikram V. A1 - Errando, M. A1 - Falcone, A. A1 - Feng, Q. A1 - Finley, J. P. A1 - Fleischhack, H. A1 - Fortson, L. A1 - Furniss, A. A1 - Griffin, S. A1 - Huetten, M. A1 - Hanna, D. A1 - Holder, J. A1 - Johnson, C. A. A1 - Kaaret, P. A1 - Kar, P. A1 - Kelley-Hoskins, N. A1 - Kertzman, M. A1 - Kieda, D. A1 - Krause, M. A1 - Kumar, S. A1 - Lang, M. J. A1 - Maier, G. A1 - McArthur, S. A1 - McCann, A. A1 - Moriarty, P. A1 - Mukherjee, R. A1 - Nieto, D. A1 - Ong, R. A. A1 - Otte, A. N. A1 - Park, Nahee A1 - Pohl, Martin A1 - Popkow, A. A1 - Pueschel, Elisa A1 - Quinn, J. A1 - Ragan, K. A1 - Reynolds, P. T. A1 - Richards, G. T. A1 - Roache, E. A1 - Sadeh, I. A1 - Santander, M. A1 - Sembroski, G. H. A1 - Shahinyan, K. A1 - Slane, P. A1 - Staszak, D. A1 - Telezhinsky, Igor O. A1 - Trepanier, S. A1 - Tyler, J. A1 - Wakely, S. P. A1 - Weinstein, A. A1 - Weisgarber, T. A1 - Wilcox, P. A1 - Wilhelm, Alina A1 - Williams, D. A. A1 - Zitzer, B. T1 - Gamma-ray Observations of Tycho's Supernova Remnant with VERITAS and Fermi JF - The astrophysical journal : an international review of spectroscopy and astronomical physics KW - material KW - data behind figure Y1 - 2017 U6 - https://doi.org/10.3847/1538-4357/836/1/23 SN - 0004-637X SN - 1538-4357 VL - 836 IS - 1 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Archambault, S. A1 - Arlen, T. A1 - Aune, T. A1 - Behera, B. A1 - Beilicke, M. A1 - Benbow, W. A1 - Bird, R. A1 - Bouvier, A. A1 - Buckley, J. H. A1 - Bugaev, V. A1 - Byrum, K. A1 - Cesarini, A. A1 - Ciupik, L. A1 - Connolly, M. P. A1 - Cui, W. A1 - Errando, M. A1 - Falcone, A. A1 - Federici, Simone A1 - Feng, Q. A1 - Finley, J. P. A1 - Fortson, L. A1 - Furniss, A. A1 - Galante, N. A1 - Gall, D. A1 - Gillanders, G. H. A1 - Griffin, S. A1 - Grube, J. A1 - Gyuk, G. A1 - Hanna, D. A1 - Holder, J. A1 - Hughes, G. A1 - Humensky, T. B. A1 - Kaaret, P. A1 - Kertzman, M. A1 - Khassen, Y. A1 - Kieda, D. A1 - Krawczynski, H. A1 - Krennrich, F. A1 - Kumar, S. A1 - Lang, M. J. A1 - Madhavan, A. S. A1 - Maier, G. A1 - Majumdar, P. A1 - McArthur, S. A1 - McCann, A. A1 - Millis, J. A1 - Moriarty, P. A1 - Mukherjee, R. A1 - de Bhroithe, A. O'Faolain A1 - Ong, R. A. A1 - Otte, A. N. A1 - Park, N. A1 - Perkins, J. S. A1 - Pohl, Martin A1 - Popkow, A. A1 - Prokoph, H. A1 - Quinn, J. A1 - Ragan, K. A1 - Reyes, L. C. A1 - Reynolds, P. T. A1 - Richards, G. T. A1 - Roache, E. A1 - Saxon, D. B. A1 - Sembroski, G. H. A1 - Smith, A. W. A1 - Staszak, D. A1 - Telezhinsky, Igor O. A1 - Theiling, M. A1 - Varlotta, A. A1 - Vassiliev, V. V. A1 - Vincent, S. A1 - Wakely, S. P. A1 - Weekes, T. C. A1 - Weinstein, A. A1 - Welsing, R. A1 - Williams, D. A. A1 - Zitzer, B. A1 - Boettcher, Markus A1 - Fegan, S. J. A1 - Fortin, P. A1 - Halpern, J. P. A1 - Kovalev, Y. Y. A1 - Lister, M. L. A1 - Liu, J. A1 - Pushkarev, A. B. A1 - Smith, P. S. T1 - Discovery of a new tev Gamma-Ray source - VER J0521+211 JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - We report the detection of a new TeV gamma-ray source, VER J0521+211, based on observations made with the VERITAS imaging atmospheric Cherenkov Telescope Array. These observations were motivated by the discovery of a cluster of >30 GeV photons in the first year of Fermi Large Area Telescope observations. VER J0521+211 is relatively bright at TeV energies, with a mean photon flux of (1.93 +/- 0.13(stat) +/- 0.78(sys)) x 10(-11) cm(-2) s(-1) above 0.2 TeV during the period of the VERITAS observations. The source is strongly variable on a daily timescale across all wavebands, from optical to TeV, with a peak flux corresponding to similar to 0.3 times the steady Crab Nebula flux at TeV energies. Follow-up observations in the optical and X-ray bands classify the newly discovered TeV source as a BL Lac-type blazar with uncertain redshift, although recent measurements suggest z = 0.108. VER J0521+211 exhibits all the defining properties of blazars in radio, optical, X-ray, and gamma-ray wavelengths. KW - BL Lacertae objects: individual (VER J0521+211) KW - gamma rays: galaxies Y1 - 2013 U6 - https://doi.org/10.1088/0004-637X/776/2/69 SN - 0004-637X SN - 1538-4357 VL - 776 IS - 2 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Archambault, S. A1 - Arlen, T. A1 - Aune, T. A1 - Beilicke, M. A1 - Benbow, W. A1 - Bird, R. A1 - Boettcher, Markus A1 - Bouvier, A. A1 - Buckley, J. H. A1 - Bugaev, V. A1 - Ciupik, L. A1 - Collins-Hughes, E. A1 - Connolly, M. P. A1 - Cui, W. A1 - Dickherber, R. A1 - Dumm, J. A1 - Errando, M. A1 - Falcone, A. A1 - Federici, Simone A1 - Feng, Q. A1 - Finley, J. P. A1 - Fortson, L. A1 - Furniss, A. A1 - Galante, N. A1 - Gall, D. A1 - Garson, A. III. A1 - Gillanders, G. H. A1 - Griffin, S. A1 - Grube, J. A1 - Gusbar, C. A1 - Gyuk, G. A1 - Hanna, D. A1 - Holder, J. A1 - Hughes, G. A1 - Kaaret, P. A1 - Kertzman, M. A1 - Khassen, Y. A1 - Kieda, D. A1 - Krawczynski, H. A1 - Lamerato, A. A1 - Lang, M. J. A1 - Li, K. A1 - Madhavan, A. S. A1 - Maier, G. A1 - Majumdar, P. A1 - McArthur, S. A1 - McCann, A. A1 - Millis, J. A1 - Moriarty, P. A1 - Mukherjee, R. A1 - Nieto, D. A1 - Ong, R. A. A1 - Orr, M. A1 - Otte, A. N. A1 - Park, N. A1 - Perkins, J. S. A1 - Pohl, Martin A1 - Popkow, A. A1 - Prokoph, H. A1 - Quinn, J. A1 - Ragan, K. A1 - Reynolds, P. T. A1 - Richards, G. T. A1 - Roache, E. A1 - Roustazadeh, P. A1 - Saxon, D. B. A1 - Sembroski, G. H. A1 - Senturk, G. D. A1 - Skole, C. A1 - Staszak, D. A1 - Telezhinsky, Igor O. A1 - Tesic, G. A1 - Theiling, M. A1 - Varlotta, A. A1 - Vassiliev, V. V. A1 - Vincent, S. A1 - Wakely, S. P. A1 - Weinstein, A. A1 - Welsing, R. A1 - Williams, D. A. A1 - Zitzer, B. T1 - Test of models of the cosmic infrared background with multiwavelength observations of the blazar 1ES 1218+30.4 IN 2009 JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - We present the results of a multi-wavelength campaign targeting the blazar 1ES 1218+30.4 with observations with the 1.3 m McGraw-Hill optical telescope, the Rossi X-ray Timing Explorer (RXTE), the Fermi Gamma-Ray Space Telescope, and the Very Energetic Radiation Imaging Telescope Array System (VERITAS). The RXTE and VERITAS observations were spread over a 13 day period and revealed clear evidence for flux variability, and a strong X-ray and gamma-ray flare on 2009 February 26 (MJD 54888). The campaign delivered a well-sampled broadband energy spectrum with simultaneous RXTE and VERITAS very high energy (VHE, > 100 GeV) observations, as well as contemporaneous optical and Fermi observations. The 1ES 1218+30.4 broadband energy spectrum-the first with simultaneous X-ray and VHE gamma-ray energy spectra-is of particular interest as the source is located at a high cosmological redshift for a VHE source (z = 0.182), leading to strong absorption of VHE gamma rays by photons from the optical/infrared extragalactic background light (EBL) via gamma VHE +gamma EBL -> e(+) e(-)pair-creation processes. We model the data with a one-zone synchrotron self-Compton (SSC) emission model and with the extragalactic absorption predicted by several recent EBL models. We find that the observations are consistent with the SSC scenario and all the EBL models considered in this work. We discuss observational and theoretical avenues to improve on the EBL constraints. KW - BL Lacertae objects: general KW - BL Lacertae objects: individual (1ES1218+30.4) KW - cosmic background radiation KW - diffuse radiation KW - galaxies: jets KW - gamma rays: galaxies Y1 - 2014 U6 - https://doi.org/10.1088/0004-637X/788/2/158 SN - 0004-637X SN - 1538-4357 VL - 788 IS - 2 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Archambault, S. A1 - Aune, T. A1 - Behera, B. A1 - Beilicke, M. A1 - Benbow, W. A1 - Berger, K. A1 - Bird, R. A1 - Biteau, Jonathan A1 - Bugaev, V. A1 - Byrum, K. A1 - Cardenzana, J. V. A1 - Cerruti, M. A1 - Chen, Xuhui A1 - Ciupik, L. A1 - Connolly, M. P. A1 - Cui, Wei A1 - Dumm, J. A1 - Errando, M. A1 - Falcone, A. A1 - Federici, Simone A1 - Feng, Q. A1 - Finley, J. P. A1 - Fleischhack, H. A1 - Fortson, L. A1 - Furniss, A. A1 - Galante, N. A1 - Gillanders, G. H. A1 - Griffin, S. A1 - Griffiths, S. T. A1 - Grube, J. A1 - Gyuk, G. A1 - Hanna, D. A1 - Holder, J. A1 - Hughes, G. A1 - Humensky, T. B. A1 - Johnson, C. A. A1 - Kaaret, P. A1 - Kertzman, M. A1 - Khassen, Y. A1 - Kieda, D. A1 - Krawczynski, H. A1 - Krennrich, F. A1 - Kumar, S. A1 - Lang, M. J. A1 - Madhavan, A. S. A1 - Maier, G. A1 - McCann, A. A1 - Meagher, K. A1 - Moriarty, P. A1 - Mukherjee, R. A1 - Nieto, Daniel A1 - Ong, R. A. A1 - Otte, A. N. A1 - Park, N. A1 - Pohl, Martin A1 - Popkow, A. A1 - Prokoph, H. A1 - Quinn, J. A1 - Ragan, K. A1 - Rajotte, J. A1 - Reyes, L. C. A1 - Reynolds, P. T. A1 - Richards, G. T. A1 - Roache, E. A1 - Sembroski, G. H. A1 - Shahinyan, K. A1 - Staszak, D. A1 - Telezhinsky, Igor O. A1 - Tucci, J. V. A1 - Tyler, J. A1 - Varlotta, A. A1 - Vassiliev, V. V. A1 - Vincent, S. A1 - Wakely, S. P. A1 - Weinstein, A. A1 - Welsing, R. A1 - Wilhelm, Alina A1 - Williams, D. A. A1 - Ackermann, Margit A1 - Ajello, M. A1 - Albert, A. A1 - Baldini, L. A1 - Bastieri, D. A1 - Bellazzini, R. A1 - Bissaldi, E. A1 - Bregeon, Johan A1 - Buehler, R. A1 - Buson, S. A1 - Caliandro, G. A. A1 - Cameron, R. A. A1 - Caraveo, P. A. A1 - Cavazzuti, E. A1 - Charles, E. A1 - Chiang, J. A1 - Ciprini, S. A1 - Claus, R. A1 - Cutini, S. A1 - de Angelis, A. A1 - de Palma, F. A1 - Dermer, C. D. A1 - Digel, S. W. A1 - Di Venere, L. A1 - Drell, P. S. A1 - Favuzzi, C. A1 - Franckowiak, A. A1 - Fusco, P. A1 - Gargano, F. A1 - Gasparrini, D. A1 - Giglietto, N. A1 - Giordano, F. A1 - Giroletti, M. A1 - Grenier, I. A. A1 - Guiriec, S. A1 - Jogler, T. A1 - Kuss, M. A1 - Larsson, S. A1 - Latronico, L. A1 - Longo, F. A1 - Loparco, F. A1 - Lubrano, P. A1 - Madejski, G. M. A1 - Mayer, M. A1 - Mazziotta, Mario Nicola A1 - Michelson, P. F. A1 - Mizuno, T. A1 - Monzani, M. E. A1 - Morselli, Aldo A1 - Murgia, S. A1 - Nuss, E. A1 - Ohsugi, T. A1 - Ormes, J. F. A1 - Paneque, D. A1 - Perkins, J. S. A1 - Piron, F. A1 - Pivato, G. A1 - Raino, S. A1 - Razzano, M. A1 - Reimer, A. A1 - Reimer, Olaf A1 - Ritz, S. A1 - Schaal, M. A1 - Sgro, C. A1 - Siskind, E. J. A1 - Spinelli, P. A1 - Takahashi, H. A1 - Tibaldo, L. A1 - Tinivella, M. A1 - Troja, E. A1 - Vianello, G. A1 - Werner, M. A1 - Wood, M. T1 - Deep broadband observations of the distant gamma-ray blazar PKS 1424+240 JF - The astrophysical journal : an international review of spectroscopy and astronomical physics ; Part 2, Letters N2 - We present deep VERITAS observations of the blazar PKS 1424+240, along with contemporaneous Fermi Large Area Telescope, Swift X-ray Telescope, and Swift UV Optical Telescope data between 2009 February 19 and 2013 June 8. This blazar resides at a redshift of z >= 0.6035, displaying a significantly attenuated gamma-ray flux above 100 GeV due to photon absorption via pair-production with the extragalactic background light. We present more than 100 hr of VERITAS observations over three years, a multiwavelength light curve, and the contemporaneous spectral energy distributions. The source shows a higher flux of (2.1 +/- 0.3) x 10(-7) photons m(-2) s(-1) above 120 GeV in 2009 and 2011 as compared to the flux measured in 2013, corresponding to (1.02 +/- 0.08) x 10-7 photons m(-2) s(-1) above 120 GeV. The measured differential very high energy (VHE; E >= 100 GeV) spectral indices are Gamma = 3.8 +/- 0.3, 4.3 +/- 0.6 and 4.5 +/- 0.2 in 2009, 2011, and 2013, respectively. No significant spectral change across the observation epochs is detected. We find no evidence for variability at gamma-ray opacities of greater than tau = 2, where it is postulated that any variability would be small and occur on timescales longer than a year if hadronic cosmic-ray interactions with extragalactic photon fields provide a secondary VHE photon flux. The data cannot rule out such variability due to low statistics. KW - BL Lacertae objects: individual (PKS 1424+240)-cosmic background radiation KW - gamma rays: galaxies Y1 - 2014 U6 - https://doi.org/10.1088/2041-8205/785/1/L16 SN - 2041-8205 SN - 2041-8213 VL - 785 IS - 1 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Archambault, S. A1 - Beilicke, M. A1 - Benbow, W. A1 - Berger, K. A1 - Bird, R. A1 - Bouvier, A. A1 - Buckley, J. H. A1 - Bugaev, V. A1 - Byrum, K. A1 - Cerruti, M. A1 - Chen, Xuhui A1 - Ciupik, L. A1 - Connolly, M. P. A1 - Cui, W. A1 - Duke, C. A1 - Dumm, J. A1 - Errando, M. A1 - Falcone, A. A1 - Federici, Simone A1 - Feng, Q. A1 - Finley, J. P. A1 - Fortson, L. A1 - Furniss, A. A1 - Galante, N. A1 - Gillanders, G. H. A1 - Griffin, S. A1 - Griffiths, S. T. A1 - Grube, J. A1 - Gyuk, G. A1 - Hanna, D. A1 - Holder, J. A1 - Hughes, G. A1 - Humensky, T. B. A1 - Kaaret, P. A1 - Kertzman, M. A1 - Khassen, Y. A1 - Kieda, D. A1 - Krawczynski, H. A1 - Lang, M. J. A1 - Madhavan, A. S. A1 - Maier, G. A1 - Majumdar, P. A1 - McArthur, S. A1 - McCann, A. A1 - Moriarty, P. A1 - Mukherjee, R. A1 - Nieto, D. A1 - de Bhroithe, A. O'Faolain A1 - Ong, R. A. A1 - Otte, A. N. A1 - Pandel, D. A1 - Park, N. A1 - Perkins, J. S. A1 - Pohl, Martin A1 - Popkow, A. A1 - Prokoph, H. A1 - Quinn, J. A1 - Ragan, K. A1 - Rajotte, J. A1 - Reyes, L. C. A1 - Reynolds, P. T. A1 - Richards, G. T. A1 - Roache, E. A1 - Sembroski, G. H. A1 - Sheidaei, F. A1 - Smith, A. W. A1 - Staszak, D. A1 - Telezhinsky, Igor O. A1 - Theiling, M. A1 - Tucci, J. V. A1 - Tyler, J. A1 - Varlotta, A. A1 - Vincent, S. A1 - Wakely, S. P. A1 - Weekes, T. C. A1 - Weinstein, A. A1 - Williams, D. A. A1 - Zitzer, B. A1 - McCollough, M. L. T1 - Veritas observatons of the microquasar cygnus X-3 JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - We report results from TeV gamma-ray observations of the microquasar Cygnus X-3. The observations were made with the Very Energetic Radiation Imaging Telescope Array System (VERITAS) over a time period from 2007 June 11 to 2011 November 28. VERITAS is most sensitive to gamma rays at energies between 85 GeV and 30 TeV. The effective exposure time amounts to a total of about 44 hr, with the observations covering six distinct radio/X-ray states of the object. No significant TeV gamma-ray emission was detected in any of the states, nor with all observations combined. The lack of a positive signal, especially in the states where GeV gamma rays were detected, places constraints on TeV gamma-ray production in Cygnus X-3. We discuss the implications of the results. KW - acceleration of particles KW - binaries: close KW - gamma rays: stars KW - X-rays: individual (Cygnus X-3) Y1 - 2013 U6 - https://doi.org/10.1088/0004-637X/779/2/150 SN - 0004-637X SN - 1538-4357 VL - 779 IS - 2 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Archer, A. A1 - Barnacka, Anna A1 - Beilicke, M. A1 - Benbow, W. A1 - Berger, K. A1 - Bird, R. A1 - Biteau, Jonathan A1 - Buckley, J. H. A1 - Bugaev, V. A1 - Byrum, K. A1 - Cardenzana, J. V. A1 - Cerruti, M. A1 - Chen, W. A1 - Chen, Xiaoming A1 - Ciupik, L. A1 - Connolly, M. P. A1 - Cui, W. A1 - Dickinson, H. J. A1 - Dumm, J. A1 - Eisch, J. D. A1 - Falcone, A. A1 - Federici, Simone A1 - Feng, Q. A1 - Finley, J. P. A1 - Fleischhack, H. A1 - Fortson, L. A1 - Furniss, A. A1 - Galante, N. A1 - Griffin, S. A1 - Griffiths, S. T. A1 - Grube, J. A1 - Gyuk, G. A1 - Hakansson, Nils A1 - Hanna, D. A1 - Holder, J. A1 - Hughes, G. A1 - Johnson, C. A. A1 - Kaaret, P. A1 - Kar, P. A1 - Kertzman, M. A1 - Khassen, Y. A1 - Kieda, D. A1 - Krawczynski, H. A1 - Kumar, S. A1 - Lang, M. J. A1 - Maier, G. A1 - McArthur, S. A1 - McCann, A. A1 - Meagher, K. A1 - Moriarty, P. A1 - Mukherjee, R. A1 - Nieto, D. A1 - Ong, R. A. A1 - Otte, A. N. A1 - Park, N. A1 - Perkins, J. S. A1 - Pohl, Manuela A1 - Popkow, A. A1 - Prokoph, H. A1 - Pueschel, Elisa A1 - Quinn, J. A1 - Ragan, K. A1 - Rajotte, J. A1 - Reyes, L. C. A1 - Reynolds, P. T. A1 - Richards, G. T. A1 - Roache, E. A1 - Sembroski, G. H. A1 - Shahinyan, K. A1 - Smith, A. W. A1 - Staszak, D. A1 - Telezhinsky, Igor O. A1 - Tucci, J. V. A1 - Tyler, J. A1 - Varlotta, A. A1 - Vincent, S. A1 - Wakely, S. P. A1 - Weinstein, A. A1 - Welsing, R. A1 - Wilhelm, Alina A1 - Williams, D. A. A1 - Zajczyk, A. A1 - Zitzer, B. T1 - Very-high energy observations of the galactic center region by veritas IN 2010-2012 JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - The Galactic center is an interesting region for high-energy (0.1-100 GeV) and very-high-energy (E > 100 GeV) gamma-ray observations. Potential sources of GeV/TeV gamma-ray emission have been suggested, e.g., the accretion of matter onto the supermassive black hole, cosmic rays from a nearby supernova remnant (e.g., Sgr A East), particle acceleration in a plerion, or the annihilation of dark matter particles. The Galactic center has been detected by EGRET and by Fermi/LAT in the MeV/GeV energy band. At TeV energies, the Galactic center was detected with moderate significance by the CANGAROO and Whipple 10 m telescopes and with high significance by H.E.S.S., MAGIC, and VERITAS. We present the results from three years of VERITAS observations conducted at large zenith angles resulting in a detection of the Galactic center on the level of 18 standard deviations at energies above similar to 2.5 TeV. The energy spectrum is derived and is found to be compatible with hadronic, leptonic, and hybrid emission models discussed in the literature. Future, more detailed measurements of the high-energy cutoff and better constraints on the high-energy flux variability will help to refine and/or disentangle the individual models. KW - astroparticle physics KW - black hole physics KW - Galaxy: center KW - gamma rays: galaxies KW - methods: data analysis KW - radiation mechanisms: non-thermal Y1 - 2014 U6 - https://doi.org/10.1088/0004-637X/790/2/149 SN - 0004-637X SN - 1538-4357 VL - 790 IS - 2 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Archer, A. A1 - Benbow, W. A1 - Bird, R. A1 - Brose, Robert A1 - Buchovecky, M. A1 - Buckley, J. H. A1 - Bugaev, V. A1 - Connolly, M. P. A1 - Cui, W. A1 - Daniel, M. K. A1 - Feng, Q. A1 - Finley, J. P. A1 - Fortson, L. A1 - Furniss, A. A1 - Gillanders, G. A1 - Huetten, M. A1 - Hanna, D. A1 - Hervet, O. A1 - Holder, J. A1 - Hughes, G. A1 - Humensky, T. B. A1 - Johnson, C. A. A1 - Kaaret, P. A1 - Kar, P. A1 - Kelley-Hoskins, N. A1 - Kertzman, M. A1 - Kieda, D. A1 - Krause, M. A1 - Krennrich, F. A1 - Kumar, S. A1 - Lang, M. J. A1 - Lin, T. T. Y. A1 - Maier, G. A1 - McArthur, S. A1 - Moriarty, P. A1 - Mukherjee, R. A1 - Ong, R. A. A1 - Otte, A. N. A1 - Petrashyk, A. A1 - Pohl, M. A1 - Pueschel, Elisa A1 - Quinn, J. A1 - Ragan, K. A1 - Reynolds, P. T. A1 - Richards, G. T. A1 - Roache, E. A1 - Rulten, C. A1 - Sadeh, I. A1 - Santander, M. A1 - Sembroski, G. H. A1 - Staszak, D. A1 - Sushch, I. A1 - Wakely, S. P. A1 - Wells, R. M. A1 - Wilcox, P. A1 - Wilhelm, Alina A1 - Williams, D. A. A1 - Williamson, T. J. A1 - Zitzer, B. T1 - Measurement of cosmic-ray electrons at TeV energies by VERITAS JF - Physical review : D, Particles, fields, gravitation, and cosmology N2 - Cosmic-ray electrons and positrons (CREs) at GeV-TeV energies are a unique probe of our local Galactic neighborhood. CREs lose energy rapidly via synchrotron radiation and inverse-Compton scattering processes while propagating within the Galaxy, and these losses limit their propagation distance. For electrons with TeV energies, the limit is on the order of a kiloparsec. Within that distance, there are only a few known astrophysical objects capable of accelerating electrons to such high energies. It is also possible that the CREs are the products of the annihilation or decay of heavy dark matter (DM) particles. VERITAS, an array of imaging air Cherenkov telescopes in southern Arizona, is primarily utilized for gamma-ray astronomy but also simultaneously collects CREs during all observations. We describe our methods of identifying CREs in VERITAS data and present an energy spectrum, extending from 300 GeV to 5 TeV, obtained from approximately 300 hours of observations. A single power-law fit is ruled out in VERITAS data. We find that the spectrum of CREs is consistent with a broken power law, with a break energy at 710 +/- 40(stat) +/- 140(syst) GeV. Y1 - 2018 U6 - https://doi.org/10.1103/PhysRevD.98.062004 SN - 2470-0010 SN - 2470-0029 VL - 98 IS - 6 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Archer, A. A1 - Benbow, W. A1 - Bird, R. A1 - Brose, Robert A1 - Buchovecky, M. A1 - Bugaev, V. A1 - Connolly, M. P. A1 - Cui, W. A1 - Daniel, M. K. A1 - Falcone, A. A1 - Feng, Q. A1 - Finley, J. P. A1 - Fleischhack, H. A1 - Fortson, L. A1 - Furniss, A. A1 - Hanna, D. A1 - Hervet, O. A1 - Holder, J. A1 - Hughes, G. A1 - Humensky, T. B. A1 - Hutten, M. A1 - Johnson, C. A. A1 - Kaaret, P. A1 - Kelley-Hoskins, N. A1 - Kieda, D. A1 - Krause, M. A1 - Krennrich, F. A1 - Kumar, S. A1 - Lang, M. J. A1 - Maier, G. A1 - McArthur, S. A1 - Moriarty, P. A1 - Mukherjee, R. A1 - Nieto, D. A1 - Ong, R. A. A1 - Otte, A. N. A1 - Park, N. A1 - Petrashyk, A. A1 - Pohl, Martin A1 - Popkow, A. A1 - Pueschel, Elisa A1 - Quinn, J. A1 - Ragan, K. A1 - Reynolds, P. T. A1 - Richards, G. T. A1 - Roache, E. A1 - Rulten, C. A1 - Sadeh, I. A1 - Tyler, J. A1 - Wakely, S. P. A1 - Weiner, O. M. A1 - Wilcox, P. A1 - Wilhelm, Alina A1 - Williams, D. A. A1 - Wissel, S. A. A1 - Zitzer, B. T1 - Measurement of the iron spectrum in cosmic rays by VERITAS JF - Physical review : D, Particles, fields, gravitation, and cosmology N2 - We present a new measurement of the energy spectrum of iron nuclei in cosmic rays from 20 TeV to 500 TeV; The measurement makes use of a template-based analysis method, which, for the first time, is applied to the energy reconstruction of iron-induced air showers recorded by the VERITAS array of imaging atmospheric Cherenkov telescopes. The event selection makes use of the direct Cherenkov light which is emitted by charged particles before the first interaction, as well as other parameters related to the shape of the recorded air shower images. The measured spectrum is well described by a power law dF/dE = f(0) center dot (E/E-0)(-gamma) over the full energy range, with gamma = 2.82 +/- 0.30(stat)(-0.27)(+0.24)(syst) and f(0) = (4.82 +/- 0.98(stat)(-2.70)(+2.12)(syst)) x 10(-7) m(-2) s(-1) TeV-1 sr(-1) at E-0 = 50 TeV, with no indication of a cutoff or spectral break. The measured differential flux is compatible with previous results, with improved statistical uncertainty at the highest energies. Y1 - 2018 U6 - https://doi.org/10.1103/PhysRevD.98.022009 SN - 2470-0010 SN - 2470-0029 VL - 98 IS - 2 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Archer, A. A1 - Benbow, W. A1 - Bird, R. A1 - Buchovecky, M. A1 - Buckley, J. H. A1 - Bugaev, V. A1 - Byrum, K. A1 - Cardenzana, J. V. A1 - Cerruti, M. A1 - Chen, Xuhui A1 - Ciupik, L. A1 - Collins-Hughes, E. A1 - Connolly, M. P. A1 - Eisch, J. D. A1 - Falcone, A. A1 - Feng, Q. A1 - Finley, J. P. A1 - Fleischhack, H. A1 - Flinders, A. A1 - Fortson, L. A1 - Furniss, A. A1 - Gillanders, G. H. A1 - Griffin, S. A1 - Grube, J. A1 - Gyuk, G. A1 - Hakansson, Nils A1 - Hanna, D. A1 - Holder, J. A1 - Humensky, T. B. A1 - Huetten, M. A1 - Johnson, C. A. A1 - Kaaret, P. A1 - Kar, P. A1 - Kelley-Hoskins, N. A1 - Kertzman, M. A1 - Kieda, D. A1 - Krause, M. A1 - Krennrich, F. A1 - Kumar, S. A1 - Lang, M. J. A1 - McArthur, S. A1 - McCann, A. A1 - Meagher, K. A1 - Millis, J. A1 - Moriarty, P. A1 - Mukherjee, R. A1 - Nieto, D. A1 - Ong, R. A. A1 - Park, N. A1 - Pelassa, V. A1 - Pohl, Martin A1 - Popkow, A. A1 - Pueschel, Elisa A1 - Quinn, J. A1 - Ragan, K. A1 - Ratliff, G. A1 - Reynolds, P. T. A1 - Richards, G. T. A1 - Roache, E. A1 - Rousselle, J. A1 - Santander, M. A1 - Sembroski, G. H. A1 - Shahinyan, K. A1 - Smith, A. W. A1 - Staszak, D. A1 - Telezhinsky, Igor O. A1 - Tucci, J. V. A1 - Tyler, J. A1 - Vassiliev, V. V. A1 - Wakely, S. P. A1 - Weiner, O. M. A1 - Weinstein, A. A1 - Wilhelm, Alina A1 - Williams, D. A. A1 - Zitzer, B. A1 - Yusef-Zadeh, F. T1 - TEV GAMMA-RAY OBSERVATIONS OF THE GALACTIC CENTER RIDGE BY VERITAS JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - The Galactic Center ridge has been observed extensively in the past by both GeV and TeV gamma-ray instruments revealing a wealth of structure, including a diffuse component and the point sources G0.9+0.1 (a composite supernova remnant) and Sgr A* (believed to be associated with the supermassive black hole located at the center of our Galaxy). Previous very high energy (VHE) gamma-ray observations with the H.E.S.S.. experiment have also detected an extended TeV gamma-ray component along the Galactic plane in the >300 GeV gamma-ray regime. Here we report on observations of the Galactic Center ridge from 2010 to 2014 by the VERITAS telescope array in the >2 TeV energy range. From these observations we (1) provide improved measurements of the differential energy spectrum for Sgr A* in the >2 TeV gamma-ray regime, (2) provide a detection in the >2 TeV gamma-ray emission from the composite SNR G0.9+0.1 and an improved determination of its multi-TeV gamma-ray energy spectrum, and. (3) report on the detection of VER J1746-289, a localized enhancement of >2 TeV gamma-ray emission along the Galactic plane. KW - Galaxy: center KW - gamma rays: general KW - supernovae: individual (G0.9+0.1) Y1 - 2016 U6 - https://doi.org/10.3847/0004-637X/821/2/129 SN - 0004-637X SN - 1538-4357 VL - 821 SP - 162 EP - 167 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Archer, A. A1 - Benbow, Wystan A1 - Bird, Ralph A1 - Brose, Robert A1 - Buchovecky, M. A1 - Buckley, J. H. A1 - Chromey, A. J. A1 - Cui, Wei A1 - Falcone, A. A1 - Feng, Qi A1 - Finley, J. P. A1 - Fortson, Lucy A1 - Furniss, Amy A1 - Gent, A. A1 - Gueta, O. A1 - Hanna, David A1 - Hassan, T. A1 - Hervet, Olivier A1 - Holder, J. A1 - Hughes, G. A1 - Humensky, T. B. A1 - Johnson, Caitlin A. A1 - Kaaret, Philip A1 - Kar, P. A1 - Kelley-Hoskins, N. A1 - Kertzman, M. A1 - Kieda, David A1 - Krennrich, F. A1 - Kumar, S. A1 - Lang, M. J. A1 - Lin, T. T. Y. A1 - McCann, A. A1 - Moriarty, P. A1 - Mukherjee, Reshmi A1 - Ong, R. A. A1 - Otte, Adam Nepomuk A1 - Pandel, D. A1 - Park, N. A1 - Petrashyk, A. A1 - Pohl, Martin A1 - Pueschel, Elisa A1 - Quinn, J. A1 - Ragan, K. A1 - Richards, Gregory T. A1 - Roache, E. A1 - Sadeh, I A1 - Santander, Marcos A1 - Scott, S. S. A1 - Sembroski, G. H. A1 - Shahinyan, Karlen A1 - Sushch, Iurii A1 - Tyler, J. A1 - Wakely, S. P. A1 - Weinstein, A. A1 - Wells, R. M. A1 - Wilcox, P. A1 - Wilhelm, Alina A1 - Williams, D. A. A1 - Williamson, T. J. A1 - Zitzer, B. T1 - A Search for Pulsed Very High-energy Gamma-Rays from 13 Young Pulsars in Archival VERITAS Data JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - We conduct a search for periodic emission in the very high-energy (VHE) gamma-ray band (E > 100 GeV) from a total of 13 pulsars in an archival VERITAS data set with a total exposure of over 450 hr. The set of pulsars includes many of the brightest young gamma-ray pulsars visible in the Northern Hemisphere. The data analysis resulted in nondetections of pulsed VHE gamma-rays from each pulsar. Upper limits on a potential VHE gamma-ray flux are derived at the 95% confidence level above three energy thresholds using two methods. These are the first such searches for pulsed VHE emission from each of the pulsars, and the obtained limits constrain a possible flux component manifesting at VHEs as is seen for the Crab pulsar. KW - gamma rays: general KW - pulsars: general KW - stars: neutron Y1 - 2019 U6 - https://doi.org/10.3847/1538-4357/ab14f4 SN - 0004-637X SN - 1538-4357 VL - 876 IS - 2 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Archer, A. A1 - Benbow, Wystan A1 - Bird, Ralph A1 - Brose, Robert A1 - Buchovecky, M. A1 - Bugaev, V A1 - Cui, Wei A1 - Danie, M. K. A1 - Falcone, A. A1 - Feng, Qi A1 - Finley, John P. A1 - Flinders, A. A1 - Fortson, L. A1 - Furniss, Amy A1 - Gillanders, Gerard H. A1 - Huttens, M. A1 - Hanna, David A1 - Hervet, O. A1 - Holder, J. A1 - Hughes, G. A1 - Humensky, T. B. A1 - Johnson, Caitlin A. A1 - Kaaret, Philip A1 - Kar, P. A1 - Kelley-Hoskins, N. A1 - Kieda, David A1 - Krause, Maria A1 - Krennrich, F. A1 - Kumar, S. A1 - Lang, M. J. A1 - Lin, T. T. Y. A1 - McArthur, S. A1 - Moriarty, P. A1 - Mukherjee, Reshmi A1 - Nieto, Daniel A1 - Ong, R. A. A1 - Otte, A. N. A1 - Park, Nahee A1 - Petrashyk, A. A1 - Pohl, Martin A1 - Popkow, Alexis A1 - Pueschel, Elisa A1 - Quinn, J. A1 - Ragan, K. A1 - Reynold, P. T. A1 - Richards, Gregory T. A1 - Roache, E. A1 - Rulten, C. A1 - Sadeh, I A1 - Sembroski, G. H. A1 - Shahinyan, Karlen A1 - Tyler, J. A1 - Wakely, S. P. A1 - Weiner, O. M. A1 - Weinstein, A. A1 - Wells, R. M. A1 - Wilcox, P. A1 - Wilhelm, Alina A1 - Williams, David A. A1 - Brisken, W. F. A1 - Pontrelli, P. T1 - HESS J1943+213 BT - An extreme blazar shining through the galactic plane JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - HESS J1943+213 is a very high energy (VHE; > 100 GeV) gamma-ray source in the direction of the Galactic plane. Studies exploring the classification of the source are converging toward its identification as an extreme synchrotron BL Lac object. Here we present 38 hr of VERITAS observations of HESS J1943+213 taken over 2 yr. The source is detected with a significance of similar to 20 standard deviations, showing a remarkably stable flux and spectrum in VHE gamma-rays. Multifrequency Very Long Baseline Array (VLBA) observations of the source confirm the extended, jet-like structure previously found in the 1.6 GHz band with the European VLBI Network and detect this component in the 4.6 and 7.3 GHz bands. The radio spectral indices of the core and the jet and the level of polarization derived from the VLBA observations are in a range typical for blazars. Data from VERITAS, Fermi-LAT, Swift-XRT, the FLWO 48 ' telescope, and archival infrared and hard X-ray observations are used to construct and model the spectral energy distribution (SED) of the source with a synchrotron self-Compton model. The well-measured gamma-ray peak of the SED with VERITAS and Fermi-LAT provides constraining upper limits on the source redshift. Possible contribution of secondary gamma-rays from ultra-high-energy cosmic-ray-initiated electromagnetic cascades to the gamma-ray emission is explored, finding that only a segment of the VHE spectrum can be accommodated with this process. A variability search is performed across X-ray and gamma-ray bands. No statistically significant flux or spectral variability is detected. KW - astroparticle physics KW - BL Lacertae objects: individual (HESS J1943+213, VER J1943+213) KW - galaxies: active KW - galaxies: jets KW - galaxies: nuclei KW - gamma rays: galaxies Y1 - 2018 U6 - https://doi.org/10.3847/1538-4357/aacbd0 SN - 0004-637X SN - 1538-4357 VL - 862 IS - 1 PB - IOP Publ. Ltd. CY - Bristol ER - TY - THES A1 - Arentsen, Anke T1 - Galactic archaeology with the oldest stars in the Milky Way N2 - In einer dunklen Nacht kann man tausende Sterne sehen. All diese Sterne befinden sich innerhalb der Milchstraße, unsere Heimatgalaxie. Nicht alle Sterne sind gleich, sie können zum Beispiel unterschiedliche Größen, Massen, Temperaturen und Alter haben. Die schwereren Sterne leben (aus astronomischer Sicht) nicht lange, nur wenige Millionen Jahren, aber Sterne kleiner als die Sonne können mehr als zehn Milliarden Jahren alt werden. Kleine Sterne die ganz am Anfang des Universums entstanden sind leuchten immer noch. Diese uralten Sterne sind sehr hilfreich um mehr über das frühe Universum, die erste Sterne und die Geschichte der Milchstraße zu erfahren. Aber wie erkennt man uralte Sterne? Anhand ihrer chemischen Fingerabdrücke! Am Anfang des Universums gab es nur zwei chemische Elemente: Wasserstoff und Helium (und ein klein bisschen Lithium). Alle schwereren Elementen wie zum Beispiel Kohlenstoff, Kalzium und Eisen sind erst später innerhalb von Sternen und in Sternexplosionen entstanden. Je mehr Sternen geboren werden, sich entwickeln und explodieren, desto mehr chemische Elemente gibt es im Universum. Sterne die später entstehen werden mit einer größeren Menge an schweren Elementen, beziehungsweise einer größeren Metallizität, geboren. Im Bereich der Astronomie der sich „Galaktische Archäologie” nennt benutzt man Sterne mit unterschiedlichen Metallizitäten um die Geschichte der Milchstraße zu erforschen. In dieser Doktorarbeit liegt der Fokus auf den metallarmen Sterne, da man erwartet dass diese Sterne am ältesten sind und uns deswegen viel über die frühe Geschichte erzählen können. Bis heute haben wir noch keinen metallfreien Stern entdeckt, aber die metallärmsten Sterne geben uns wichtige Einblicke in das Leben und Sterben der ersten Sterne. Viele von diesen ältesten, metallärmsten Sternen haben unerwartet viel Kohlenstoff im Vergleich zu zum Beispiel Eisen. Diese kohlenstoffreichen, metallarmen Sterne (CEMP Sterne) erzählen uns etwas über die allerersten Sterne im Universum: sie haben relativ viel Kohlenstoff produziert. Wenn wir uns die genauen chemischen Fingerabdrücke von CEMP Sterne angucken, erzählen sie uns noch viel mehr. Aber unsere Interpretation hängt von der Annahme ab, dass der chemische Fingerabdruck sich während des Lebens eines Sternes nicht geändert hat. In dieser Dissertation werden neue Daten präsentiert die zeigen dass diese Annahme vielleicht zu einfach ist: viele extrem metallarme CEMP Sterne befinden sich in Doppelsternsystemen. Interaktion zwischen zwei Sternen in einem Doppelsternsystem könnte die Oberfläche von CEMP Sternen verschmutzt haben. Zwar wurden die meisten CEMP Sterne höchstwahrscheinlich nicht verschmutzt, aber wir sollten vorsichtig sein mit unserer Interpretation. Die CEMP Sterne und andere metallarme Sterne sind auch wichtig für unser Verständnis der frühen Geschichte der Milchstraße. Die meisten Forscher, die metallarme Sterne studieren, suchen diese Sterne im Halo der Milchstraße: einer riesigen, diffuse Komponente die ungefähr 1% der Sterne in unserer Galaxie enthält. Modelle sagen aber vorher dass die ältesten metallarmen Sterne sich im Zentrum der Milchstraße befinden (im „Bulge”). Das Zentrum ist leider, wegen großer Mengen Staub zwischen uns und dem Zentrum und einer überwältigenden Mehrheit an metallreichen Sternen, schwierig zu beobachten. Diese Dissertation präsentiert Ergebnisse des „Pristine Inner Galaxy Survey” (PIGS), einer neuen Himmelsdurchmusterung, die die ältesten Sterne im Bulge der Milchstraße sucht (und findet). PIGS benutzt Bilder mit einer Farbe, die für die Metallizität der Sterne empfindlich ist, und kann deswegen sehr effektiv die metallarmen Sterne aus Millionen anderer Sterne auswählen. Von interessanten Kandidaten wurden Spektren aufgenommen und mit zwei unabhängigen Methoden analysiert. Mit dieser Strategie hat PIGS die bislang größte Anzahl an metallarmen Sternen in der inneren Galaxie entdeckt. Ein neues Ergebnis aus den PIGS Daten ist, dass die metallärmeren Sterne langsamer um das Galaktische Zentrum drehen als die metallreichen Sterne, und dass sie mehr willkürliche Bewegung zeigen. Eine zweite wichtige Leistung von PIGS ist die Entdeckung von dutzenden CEMP Sternen in der innere Galaxie, wo vorher nur zwei bekannt waren. Die neuen Ergebnisse aus dieser Dissertation helfen uns die ersten Sterne und die Geschichte der Milchstraße besser zu verstehen. Laufende und neue Himmelsdurchmusterungen in den nächsten Jahren werden uns noch viel mehr Informationen geben: es ist eine aufregende Zeit für die Galaktische Archäologie. N2 - During a dark night, it is possible to observe thousands of stars by eye. All these stars are located within the Milky Way, our home. Not all stars are the same, they can have different sizes, masses, temperatures and ages. Heavy stars do not live long (in astronomical terms), only a few million years, but stars less massive than the Sun can get more than ten billion years old. Such small stars that formed in the beginning of the Universe still shine today. These ancient stars are very helpful to learn more about the early Universe, the First Stars and the history of the Milky Way. But how do you recognise an ancient star? Using their chemical fingerprints! In the beginning of the Universe, there were only two chemical elements: hydrogen and helium (and a tiny bit of lithium). All the heavier elements like carbon, calcium and iron were only made later within stars and their explosions. The amount of chemical elements in the Universe increases with the number of stars that are born, evolve and explode. Stars that form later are born with more heavy elements, or a greater metallicity. In the field of astronomy that is called “Galactic Archaeology”, stars of various metallicities are used to study the history of the Milky Way. In this doctoral thesis, the focus is on metal-poor stars because these are expected to be the oldest and can therefore tell us a lot about the early history of our Galaxy. Until today, we still have not discovered a metal-free star. The most metal-poor stars, however, give us important insights in the lives and deaths of the First Stars. Many of the oldest, most metal-poor stars have an unexpectedly large amount of carbon, compared to for example iron. These carbon-enhanced metal-poor (CEMP) stars tell us something about the very first stars in the Universe: they somehow produced a lot of carbon. If we look at the precise chemical fingerprints of the CEMP stars, we can learn a lot more. But our interpretation depends on the assumption that the chemical fingerprint of a star does not change during its life. In this thesis, new data is presented that shows that this assumption may be too simple: many extremely metal-poor CEMP stars are members of binary systems. Interactions between two stars in a binary system can pollute the surface of the stars. Likely not all of the CEMP stars in binary systems were actually polluted, but we should be very careful in our interpretations of the fingerprints of these stars. The CEMP stars and other metal-poor stars are also important for our understanding of the early history of the Milky Way. Most researchers who study metal-poor stars look for these stars in the halo of the Milky Way: a huge diffuse Galactic component containing about 1% of the stars in our Galaxy. However, models predict that the oldest metal-poor stars are located in the center of the Milky Way, in the bulge. The metal-poor inner Galaxy is unfortunately difficult to study due to large amounts of dust between us and the center and an overwhelming majority of metal-rich stars. This thesis presents results from the successful Pristine Inner Galaxy Survey (PIGS), a new survey looking for (and finding) the oldest stars in the bulge of the Milky Way. PIGS is using images with a specific color that is sensitive to the metallicity of stars, and can therefore efficiently select the metal-poor stars among millions of other, more metal-rich stars. The interesting candidates are followed up with spectroscopy, which is then analysed using two independent methods. With this strategy, PIGS has discovered the largest sample of metal-poor stars in the inner Galaxy to date. A new result from the PIGS data is that the metal-poor stars rotate more slowly around the Galactic center compared to the more metal-rich stars, and they show larger randomness in their motions as well. Another important contribution from PIGS is the discovery of tens of CEMP stars in the inner Galaxy, where previously only two such stars were known. The new results from this thesis help us to understand the First Stars and the early history of the Milky Way. Ongoing and future large surveys will provide us with a lot of additional data in the coming years. It is an exciting time for the field of Galactic Archaeology. T2 - Galaktische Archäologie mit den ältesten Sternen in der Milchstraße KW - astrophysics KW - stars KW - Milky Way KW - Galactic Archaeology KW - Astrophysik KW - Sterne KW - Milchstraße KW - Galaktische Archäologie Y1 - 2020 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-476022 ER - TY - THES A1 - Aretz, Sarah T1 - Entwicklung und Evaluation eines Testinstruments zur Untersuchung von Vorkenntnissen und Präkonzepten in der Kosmologie T1 - Development and evaluation of a test instrument to investigate students’ prior knowledge and conceptions in cosmology N2 - Kosmologie beschreibt die Entwicklung des Universums als Ganzes. Kosmologische Entdeckungen in Theorie und Praxis haben daher unser modernes wissenschaftliches Weltbild entscheidend ge­prägt. Die Vermittlung eines modernen Weltbildes durch Unterricht ist ein häufiger Wunsch in der naturwissenschaftlichen Bildungsdiskussion. Dennoch exis­tieren weiterhin Forschungs- und Entwicklungsbedarfe. Kosmologische Themen finden sich häufig in den Medien und sind gleichzeitig weiter vom Alltag entfernt, so dass sich hier besonders leicht wissenschaftlich inkorrekte Vorstellungen entwickeln können, die zu Problemen im Unterricht führen können. Das Ziel dieser wissenschaftlichen Arbeit ist es, zu diesem Forschungsgebiet beizutragen und die Voraussetzungen hinsichtlich vorhandener Vorkenntnisse und Präkonzepte in Kosmologie, mit denen Schülerinnen und Schüler in den Unterricht kommen, zu untersuchen und anschließend mit denen anderer Länder zu vergleichen. Dies erfolgt anhand einer qualitativen Inhaltsanalyse eines offenen Fragebogens. Auf dieser Grundlage wird schließlich ein Multiple-Choice Frage­bogen entwickelt, angewendet und evaluiert. Die Ergebnisse zeigen große Wissenslücken im Bereich der Kosmologie auf und geben erste Hin­weise auf vorhandene Unterschiede zwischen den Ländern. Es existieren ebenfalls einige teils weit verbreitete wissenschaftlich inkorrekte Vorstellungen wie beispiels­weise die Assoziation des Urknalls mit einer Explosion, der Urknall verursacht durch eine Kollision von Teilchen oder größeren Objekten, oder die Vorstellung der Ausdehnung des Universums als neue Entdeckungen und/oder Wissen. Des Weiteren gab nur etwa jeder Fünfte das korrekte Alter des Universums oder die Ausdehnung des Universums als einen der drei Belege der Urknalltheorie an, während fast 40% keinen einzigen Beleg nennen konn­ten. Für den geschlossenen Fragebogen konnten gute Hinweise für verschiedene Validitätsa­spekte herausgearbeitet werden und es existieren erste Hinweise darauf, dass der Fragebogen Wissenszu­wachs messen kann und damit wahrscheinlich zur Unter­suchung der Wirksamkeit von Lerneinhei­ten eingesetzt werden kann. Auch ein entsprechendes Modell zur Verständnisentwicklung der Aus­dehnung des Universums zeigte sich vielversprechend. Diese Arbeit liefert insgesamt einen Forschungsbeitrag zum Schülervorwissen und Vorstellungen in der Kosmologie und deren Large Scale Assessment. Dies eröffnet die Möglichkeit zukünftiger For­schungen im Bereich von Gruppenvergleichen insbesondere hinsichtlich objektiver Länderverglei­che sowie der Untersuchungen der Wirksamkeit von einzelnen Ler­neinheiten als auch Vergleiche verschiedener Lerneinheiten untereinander. N2 - Cosmology deals with the development of the universe as a whole. Cosmological discoveries in theory and observation have therefore formed our modern scientific worldview. Transferring a modern worldview through science teaching is a frequent request in science literacy discussion. Nevertheless, there is still a need for research and education development. Cosmological topics often appear in the media and, at the same time, are further away from everyday life. Thus, scientifically incorrect conceptions can develop particularly easy and can lead to problems in class. The objective of this scientific work is to contribute to this area of research and to investigate the preconditions regarding present knowledge and conceptions in cosmology, which students bring into the classroom, and to compare these with those from other countries. This is done by a qualitative analysis of an open-ended questionnaire. On this basis a multiple-choice questionnaire is developed, applied and evaluated. The results show large gaps in knowledge in the area of cosmology and provide first indications of differences between countries. There also exist some partially widespread scientifically incorrect conceptions such as the association of the Big Bang with an explosion, the Big Bang being caused by a collision of particles or bigger objects, or the idea of the expansion of the universe meaning new discoveries and/ or knowledge. Furthermore, only every fifth student mentioned the correct age of the universe or the expansion of the universe as one of the three pillars of the Big Bang theory, whereas almost 40% could not name a single evidence. For the closed questionnaire good evidence could be established for different aspects of validity. In addition, there exist first indications, that the questionnaire can measure knowledge gain and therefore can likely be used to investigate the effectiveness of learning units. Moreover, a corresponding model of the development of understanding of the expansion of the universe looked promising. This study provides research contributions to students' prior knowledge and preconceptions in cosmology and their large-scale assessment. This opens up the possibility of future research in the area of group comparisons in particular concerning objective country comparisons and investigations of the effectiveness of single learning units as well as comparisons of different learning units among each other. KW - Präkonzepte KW - Schülervorstellungen KW - Kosmologie KW - Testentwicklung KW - Verständnisentwicklungsmodell KW - preconceptions KW - students' conceptions KW - cosmology KW - development of test instrument KW - construct map Y1 - 2019 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-425421 ER - TY - JOUR A1 - Arhammar, C. A1 - Pietzsch, Annette A1 - Bock, Nicolas A1 - Holmstroem, Erik A1 - Araujo, C. Moyses A1 - Grasjo, Johan A1 - Zhao, Shuxi A1 - Green, Sara A1 - Peery, T. A1 - Hennies, Franz A1 - Amerioun, Shahrad A1 - Föhlisch, Alexander A1 - Schlappa, Justine A1 - Schmitt, Thorsten A1 - Strocov, Vladimir N. A1 - Niklasson, Gunnar A. A1 - Wallace, Duane C. A1 - Rubensson, Jan-Erik A1 - Johansson, Borje A1 - Ahuja, Rajeev C. T1 - Unveiling the complex electronic structure of amorphous metal oxides JF - Proceedings of the National Academy of Sciences of the United States of America N2 - Amorphous materials represent a large and important emerging area of material's science. Amorphous oxides are key technological oxides in applications such as a gate dielectric in Complementary metal-oxide semiconductor devices and in Silicon-Oxide-Nitride-Oxide-Silicon and TANOS (TaN-Al2O3-Si3N4-SiO2-Silicon) flash memories. These technologies are required for the high packing density of today's integrated circuits. Therefore the investigation of defect states in these structures is crucial. In this work we present X-ray synchrotron measurements, with an energy resolution which is about 5-10 times higher than is attainable with standard spectrometers, of amorphous alumina. We demonstrate that our experimental results are in agreement with calculated spectra of amorphous alumina which we have generated by stochastic quenching. This first principles method, which we have recently developed, is found to be superior to molecular dynamics in simulating the rapid gas to solid transition that takes place as this material is deposited for thin film applications. We detect and analyze in detail states in the band gap that originate from oxygen pairs. Similar states were previously found in amorphous alumina by other spectroscopic methods and were assigned to oxygen vacancies claimed to act mutually as electron and hole traps. The oxygen pairs which we probe in this work act as hole traps only and will influence the information retention in electronic devices. In amorphous silica oxygen pairs have already been found, thus they may be a feature which is characteristic also of other amorphous metal oxides. KW - stochastic quench KW - X-ray absorption spectroscopy KW - ab initio KW - coating Y1 - 2011 U6 - https://doi.org/10.1073/pnas.1019698108 SN - 0027-8424 VL - 108 IS - 16 SP - 6355 EP - 6360 PB - National Acad. of Sciences CY - Washington ER - TY - JOUR A1 - Arlen, T. A1 - Aune, T. A1 - Beilicke, M. A1 - Benbow, W. A1 - Bouvier, A. A1 - Buckley, J. H. A1 - Bugaev, V. A1 - Byrum, K. A1 - Cannon, A. A1 - Cesarini, A. A1 - Ciupik, L. A1 - Collins-Hughes, E. A1 - Connolly, M. P. A1 - Cui, W. A1 - Dickherber, R. A1 - Dumm, J. A1 - Falcone, A. A1 - Federici, S. A1 - Feng, Q. A1 - Finley, J. P. A1 - Finnegan, G. A1 - Fortson, L. A1 - Furniss, A. A1 - Galante, N. A1 - Gall, D. A1 - Godambe, S. A1 - Griffin, S. A1 - Grube, J. A1 - Gyuk, G. A1 - Holder, J. A1 - Huan, H. A1 - Hughes, G. A1 - Humensky, T. B. A1 - Imran, A. A1 - Kaaret, P. A1 - Karlsson, N. A1 - Kertzman, M. A1 - Khassen, Y. A1 - Kieda, D. A1 - Krawczynski, H. A1 - Krennrich, F. A1 - Lee, K. A1 - Madhavan, A. S. A1 - Maier, G. A1 - Majumdar, P. A1 - McArthur, S. A1 - McCann, A. A1 - Moriarty, P. A1 - Mukherjee, R. A1 - Nelson, T. A1 - de Bhroithe, A. O'Faolain A1 - Ong, R. A. A1 - Orr, M. A1 - Otte, A. N. A1 - Park, N. A1 - Perkins, J. S. A1 - Pohl, Martin A1 - Prokoph, H. A1 - Quinn, J. A1 - Ragan, K. A1 - Reyes, L. C. A1 - Reynolds, P. T. A1 - Roache, E. A1 - Ruppel, J. A1 - Saxon, D. B. A1 - Schroedter, M. A1 - Sembroski, G. H. A1 - Skole, C. A1 - Smith, A. W. A1 - Telezhinsky, Igor O. A1 - Tesic, G. A1 - Theiling, M. A1 - Thibadeau, S. A1 - Tsurusaki, K. A1 - Varlotta, A. A1 - Vivier, M. A1 - Wakely, S. P. A1 - Ward, J. E. A1 - Weinstein, A. A1 - Welsing, R. A1 - Williams, D. A. A1 - Zitzer, B. A1 - Pfrommer, C. A1 - Pinzke, A. T1 - Constraints on cosmic rays, magnetic fields, and dark matter fromgamma-ray observations of the coma cluster of galaxies with veritas and fermi JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - Observations of radio halos and relics in galaxy clusters indicate efficient electron acceleration. Protons should likewise be accelerated and, on account of weak energy losses, can accumulate, suggesting that clusters may also be sources of very high energy (VHE; E > 100 GeV) gamma-ray emission. We report here on VHE gamma-ray observations of the Coma galaxy cluster with the VERITAS array of imaging Cerenkov telescopes, with complementing Fermi Large Area Telescope observations at GeV energies. No significant gamma-ray emission from the Coma Cluster was detected. Integral flux upper limits at the 99% confidence level were measured to be on the order of (2-5) x 10(-8) photonsm(-2) s(-1) (VERITAS, >220 GeV) and similar to 2 x 10(-6) photonsm(-2) s(-1) (Fermi, 1-3GeV), respectively. We use the gamma-ray upper limits to constrain cosmic rays (CRs) and magnetic fields in Coma. Using an analytical approach, the CR-to-thermal pressure ratio is constrained to be < 16% from VERITAS data and <1.7% from Fermi data (averaged within the virial radius). These upper limits are starting to constrain the CR physics in self-consistent cosmological cluster simulations and cap the maximum CR acceleration efficiency at structure formation shocks to be <50%. Alternatively, this may argue for non-negligible CR transport processes such as CR streaming and diffusion into the outer cluster regions. Assuming that the radio-emitting electrons of the Coma halo result from hadronic CR interactions, the observations imply a lower limit on the central magnetic field in Coma of similar to(2-5.5) mu G, depending on the radial magnetic field profile and on the gamma-ray spectral index. Since these values are below those inferred by Faraday rotation measurements in Coma (for most of the parameter space), this renders the hadronic model a very plausible explanation of the Coma radio halo. Finally, since galaxy clusters are dark matter (DM) dominated, the VERITAS upper limits have been used to place constraints on the thermally averaged product of the total self-annihilation cross section and the relative velocity of the DM particles, . KW - cosmic rays KW - dark matter KW - galaxies: clusters: general KW - galaxies: clusters: individual (Coma (ACO 1656)) KW - gamma rays: galaxies: clusters KW - magnetic fields Y1 - 2012 U6 - https://doi.org/10.1088/0004-637X/757/2/123 SN - 0004-637X VL - 757 IS - 2 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Arlen, T. A1 - Aune, T. A1 - Beilicke, M. A1 - Benbow, W. A1 - Bouvier, A. A1 - Buckley, J. H. A1 - Bugaev, V. A1 - Cesarini, A. A1 - Ciupik, L. A1 - Connolly, M. P. A1 - Cui, W. A1 - Dickherber, R. A1 - Dumm, J. A1 - Errando, M. A1 - Falcone, A. A1 - Federici, S. A1 - Feng, Q. A1 - Finley, J. P. A1 - Finnegan, G. A1 - Fortson, L. A1 - Furniss, A. A1 - Galante, N. A1 - Gall, D. A1 - Griffin, S. A1 - Grube, J. A1 - Gyuk, G. A1 - Hanna, D. A1 - Holder, J. A1 - Humensky, T. B. A1 - Kaaret, P. A1 - Karlsson, N. A1 - Kertzman, M. A1 - Khassen, Y. A1 - Kieda, D. A1 - Krawczynski, H. A1 - Krennrich, F. A1 - Maier, G. A1 - Moriarty, P. A1 - Mukherjee, R. A1 - Nelson, T. A1 - de Bhroithe, A. O'Faolain A1 - Ong, R. A. A1 - Orr, M. A1 - Park, N. A1 - Perkins, J. S. A1 - Pichel, A. A1 - Pohl, Martin A1 - Prokoph, H. A1 - Quinn, J. A1 - Ragan, K. A1 - Reyes, L. C. A1 - Reynolds, P. T. A1 - Roache, E. A1 - Saxon, D. B. A1 - Schroedter, M. A1 - Sembroski, G. H. A1 - Staszak, D. A1 - Telezhinsky, Igor O. A1 - Tesic, G. A1 - Theiling, M. A1 - Tsurusaki, K. A1 - Varlotta, A. A1 - Vincent, S. A1 - Wakely, S. P. A1 - Weekes, T. C. A1 - Weinstein, A. A1 - Welsing, R. A1 - Williams, D. A. A1 - Zitzer, B. A1 - Jorstad, S. G. A1 - MacDonald, N. R. A1 - Marscher, A. P. A1 - Smith, P. S. A1 - Walker, R. C. A1 - Hovatta, T. A1 - Richards, J. A1 - Max-Moerbeck, W. A1 - Readhead, A. A1 - Lister, M. L. A1 - Kovalev, Y. Y. A1 - Pushkarev, A. B. A1 - Gurwell, M. A. A1 - Lahteenmaki, A. A1 - Nieppola, E. A1 - Tornikoski, M. A1 - Jarvela, E. T1 - Rapid TeV Gamma-Ray flaring of bl lacertae JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - We report on the detection of a very rapid TeV gamma-ray flare from BL Lacertae on 2011 June 28 with the Very Energetic Radiation Imaging Telescope Array System (VERITAS). The flaring activity was observed during a 34.6 minute exposure, when the integral flux above 200 GeV reached (3.4 +/- 0.6) x 10(-6) photons m(-2) s(-1), roughly 125% of the Crab Nebula flux measured by VERITAS. The light curve indicates that the observations missed the rising phase of the flare but covered a significant portion of the decaying phase. The exponential decay time was determined to be 13 +/- 4 minutes, making it one of the most rapid gamma-ray flares seen from a TeV blazar. The gamma-ray spectrum of BL Lacertae during the flare was soft, with a photon index of 3.6 +/- 0.4, which is in agreement with the measurement made previously by MAGIC in a lower flaring state. Contemporaneous radio observations of the source with the Very Long Baseline Array revealed the emergence of a new, superluminal component from the core around the time of the TeV gamma-ray flare, accompanied by changes in the optical polarization angle. Changes in flux also appear to have occurred at optical, UV, and GeV gamma-ray wavelengths at the time of the flare, although they are difficult to quantify precisely due to sparse coverage. A strong flare was seen at radio wavelengths roughly four months later, which might be related to the gamma-ray flaring activities. We discuss the implications of these multiwavelength results. KW - galaxies: active KW - galaxies: individual (BL Lacertae, VER J2202+422) KW - gamma rays: galaxies Y1 - 2013 U6 - https://doi.org/10.1088/0004-637X/762/2/92 SN - 0004-637X VL - 762 IS - 2 PB - IOP Publ. Ltd. CY - Bristol ER - TY - THES A1 - Arlt, Rainer T1 - Dynamowirkung und Drehimpulstransport in globnalen Akkretionsscheibenmodellen Y1 - 2000 ER - TY - JOUR A1 - Arlt, Rainer A1 - Valliappan, Senthamizh Pavai A1 - Schmiel, C. A1 - Spada, F. T1 - Sunspot positions, areas, and group tilt angles for 1611-1631 from observations by Christoph Scheiner JF - Mountain research and development N2 - Methods. In most cases, the given orientation of the ecliptic is used to set up the heliographic coordinate system for the drawings. Positions and sizes are measured manually on screen. Very early drawings have no indication of their orientation. A rotational matching using common spots of adjacent days is used in some cases, while in other cases, the assumption that images were aligned with a zenith-horizon coordinate system appeared to be the most probable. KW - Sun: activity KW - sunspots KW - history and philosophy of astronomy Y1 - 2016 U6 - https://doi.org/10.1051/0004-6361/201629000 SN - 1432-0746 VL - 595 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Armin, Ardalan A1 - Chen, Zhiming A1 - Jin, Yaocheng A1 - Zhang, Kai A1 - Huang, Fei A1 - Shoaee, Safa T1 - A Shockley-Type polymer BT - Fullerene solar cell JF - Advanced energy materials N2 - Charge extraction rate in solar cells made of blends of electron donating/accepting organic semiconductors is typically slow due to their low charge carrier mobility. This sets a limit on the active layer thickness and has hindered the industrialization of organic solar cells (OSCs). Herein, charge transport and recombination properties of an efficient polymer (NT812):fullerene blend are investigated. This system delivers power conversion efficiency of >9% even when the junction thickness is as large as 800 nm. Experimental results indicate that this material system exhibits exceptionally low bimolecular recombination constant, 800 times smaller than the diffusion-controlled electron and hole encounter rate. Comparing theoretical results based on a recently introduced modified Shockley model for fill factor, and experiments, clarifies that charge collection is nearly ideal in these solar cells even when the thickness is several hundreds of nanometer. This is the first realization of high-efficiency Shockley-type organic solar cells with junction thicknesses suitable for scaling up. KW - charge transport KW - non-Langevin recombination KW - organic solar cells KW - thick junctions Y1 - 2018 U6 - https://doi.org/10.1002/aenm.201701450 SN - 1614-6832 SN - 1614-6840 VL - 8 IS - 7 PB - Wiley-VCH CY - Weinheim ER - TY - THES A1 - Arora, Ashima T1 - Optical and electric field control of magnetism T1 - Optische und elektrische Feld Kontrolle des Magnetismus N2 - Future magnetic recording industry needs a high-density data storage technology. However, switching the magnetization of small bits requires high magnetic fields that cause excessive heat dissipation. Therefore, controlling magnetism without applying external magnetic field is an important research topic for potential applications in data storage devices with low power consumption. Among the different approaches being investigated, two of them stand out, namely i) all-optical helicity dependent switching (AO-HDS) and ii) ferroelectric control of magnetism. This thesis aims to contribute towards a better understanding of the physical processes behinds these effects as well as reporting new and exciting possibility for the optical and/or electric control of magnetic properties. Hence, the thesis contains two differentiated chapters of results; the first devoted to AO-HDS on TbFe alloys and the second to the electric field control of magnetism in an archetypal Fe/BaTiO3 system. In the first part, the scalability of the AO-HDS to small laser spot-sizes of few microns in the ferrimagnetic TbFe alloy is investigated by spatially resolving the magnetic contrast with photo-emission electron microscopy (PEEM) and X-ray magnetic circular dichroism (XMCD). The results show that the AO-HDS is a local effect within the laser spot size that occurs in the ring-shaped region in the vicinity of thermal demagnetization. Within the ring region, the helicity dependent switching occurs via thermally activated domain wall motion. Further, the thesis reports on a novel effect of thickness dependent inversion of the switching orientation. It addresses some of the important questions like the role of laser heating and the microscopic mechanism driving AO-HDS. The second part of the thesis focuses on the electric field control of magnetism in an artificial multiferroic heterostructure. The sample consists of an Fe wedge with thickness varying between 0:5 nm and 3 nm, deposited on top of a ferroelectric and ferroelastic BaTiO3 [001]-oriented single crystal substrate. Here, the magnetic contrast is imaged via PEEM and XMCD as a function of out-of-plane voltage. The results show the evidence of the electric field control of superparamagnetism mediated by a ferroelastic modification of the magnetic anisotropy. The changes in the magnetoelastic anisotropy drive the transition from the superparamagnetic to superferromagnetic state at localized sample positions. N2 - Die Herstellung zukünftiger magnetischer Datenspeicher erfordert eine hohe Speicherdichte mit entsprechend kleinen Bits. Das Schalten der Magnetisierung kleiner Strukturen benötigt jedoch starke Magnetfelder, die einen hohen Energieverbrauch und Wärmeeintrag verursachen. Daher ist das Schalten von Magnetismus ohne Anlegen eines externen Magnetfeldes ein wichtiges Forschungsthema für potentielle Anwendungen in der Datenspeicherung mit geringem Stromverbrauch. Unter den verschiedenen Ansätzen, die verfolgt werden, heben sich zwei hervor, nämlich i) rein optisches helizitätsabhängiges Schalten (AO-HDS) und ii) magnetoelektrische Kontrolle von Magnetismus. Diese Arbeit soll zu einem besseren Verständnis der physikalischen Prozesse beitragen, die hinter diesen Effekten stehen, sowie neue und aufregende Möglichkeiten für die optische und/ oder elektrische Kontrolle magnetischer Eigenschaften aufzeigen. Daher sind die Ergebnisse dieser Arbeit in zwei Kapitel gegliedert; das erste befasst sich mit dem helizitätsabhängigen optischen Schalten in Eisen-Terbium Legierungen und das zweite Kapitel widmet sich der magnetoelektrischen Kopplung in Hybridsystemen, bestehend aus einer ferromagnetischen Eisenschicht welche auf ferroelektrischen Bariumtitanat gewachsen wurde. Im ersten Kapitel wird die Skalierbarkeit des helizitätsabhängigen optischen Schaltens in ferrimagnetischen Eisen-Terbium Legierungen mit Laserspotgrößen im Mikrometer Bereich untersucht. Photoelektronenmikroskopie (PEEM) in Kombination mit magnetischem Röntgendichroismus (XMCD) wird verwendet um die resultierende Magnetisierung hochaufgelöst abzubilden. Die Ergebnisse zeigen, dass helizitätsabhängiges optisches Schalten ein lokaler Effekt innerhalb des Laserspots ist, der in der ringförmigen Region in der Nähe der thermischen Entmagnetisierung auftritt. Innerhalb der Ringregion erfolgt die Umkehr der Magnetisierung über thermisch aktivierte Domänenwandbewegung. Des Weiteren berichtet die Arbeit über einen neuartigen Effekt der die Helizitätsabhängigkeit mit zunehmender Schichtdicke umkehrt. Auch werden wichtigen Fragen wie der Rolle thermischer Effekt oder die mikroskopische Ursache helizitätsabhängigen Schaltens beleuchtet. Der zweite Teil der Arbeit konzentriert sich auf die elektrische Kontrolle des Magnetismus in einer künstlichen multiferroischen Heterostruktur. Die Probe besteht aus einem Eisen-Keil mit einer Dicke zwischen 0:5 nm und 3 nm, der auf einem ferroelektrischen und ferroelastischen Bariumtitanat abgeschieden ist. Hier wird der magnetische Kontrast als Funktion des elektrischen Feldes untersucht. Die Ergebnisse belegen die Möglichkeit superparamagnetische Bereiche per elektrischen Feld zu steuern. Die magnetelektrische Kopplung erfolgt durch eine ferroelastische Modifikation der magnetischen Anisotropie. Die Änderungen in der magnetoelastischen Anisotropie erlauben elektrisches Schalten zwischen dem superparamagnetischen zu dem superferromagnetischen Zustand. KW - magnetism KW - X-ray magnetic circular dichroism (XMCD) KW - all-optical helicity dependent switching KW - multiferroic heterostructure KW - photo-emission electron microscopy (PEEM) KW - magnetischem Röntgendichroismus (XMCD) KW - Photoelektronenmikroskopie (PEEM) KW - Magnetismus KW - multiferroischen Heterostruktur KW - rein optisches helizitätsabhängiges Schalten (AO-HDS) Y1 - 2018 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-421479 ER - TY - JOUR A1 - Arora, Ashima A1 - Mawass, Mohamad-Assaad A1 - Sandig, Oliver A1 - Luo, Chen A1 - Uenal, Ahmet A. A1 - Radu, Florin A1 - Valencia, Sergio A1 - Kronast, Florian T1 - Spatially resolved investigation of all optical magnetization switching in TbFe alloys JF - Scientific reports N2 - Optical control of magnetization using femtosecond laser without applying any external magnetic field offers the advantage of switching magnetic states at ultrashort time scales. Recently, all-optical helicity-dependent switching (AO-HDS) has drawn a significant attention for potential information and data storage device applications. In this work, we employ element and magnetization sensitive photoemission electron microscopy (PEEM) to investigate the role of heating in AO-HDS for thin films of the rare-earth transition-metal alloy TbFe. Spatially resolved measurements in a 3–5 μm sized stationary laser spot demonstrate that AO-HDS is a local phenomenon in the vicinity of thermal demagnetization in a ‘ring’ shaped region. The efficiency of AO-HDS further depends on a local temperature profile around the demagnetized region and thermally activated domain wall motion. We also demonstrate that the thickness of the film determines the preferential switching direction for a particular helicity. Y1 - 2017 U6 - https://doi.org/10.1038/s41598-017-09615-1 SN - 2045-2322 VL - 7 PB - Nature Publ. Group CY - London ER - TY - JOUR A1 - Arridge, Christopher S. A1 - Achilleos, N. A1 - Agarwal, Jessica A1 - Agnor, C. B. A1 - Ambrosi, R. A1 - Andre, N. A1 - Badman, S. V. A1 - Baines, K. A1 - Banfield, D. A1 - Barthelemy, M. A1 - Bisi, M. M. A1 - Blum, J. A1 - Bocanegra-Bahamon, T. A1 - Bonfond, B. A1 - Bracken, C. A1 - Brandt, P. A1 - Briand, C. A1 - Briois, C. A1 - Brooks, S. A1 - Castillo-Rogez, J. A1 - Cavalie, T. A1 - Christophe, B. A1 - Coates, Andrew J. A1 - Collinson, G. A1 - Cooper, John F. A1 - Costa-Sitja, M. A1 - Courtin, R. A1 - Daglis, I. A. A1 - De Pater, Imke A1 - Desai, M. A1 - Dirkx, D. A1 - Dougherty, M. K. A1 - Ebert, R. W. A1 - Filacchione, Gianrico A1 - Fletcher, Leigh N. A1 - Fortney, J. A1 - Gerth, I. A1 - Grassi, D. A1 - Grodent, D. A1 - Grün, Eberhard A1 - Gustin, J. A1 - Hedman, M. A1 - Helled, R. A1 - Henri, P. A1 - Hess, Sebastien A1 - Hillier, J. K. A1 - Hofstadter, M. H. A1 - Holme, R. A1 - Horanyi, M. A1 - Hospodarsky, George B. A1 - Hsu, S. A1 - Irwin, P. A1 - Jackman, C. M. A1 - Karatekin, O. A1 - Kempf, Sascha A1 - Khalisi, E. A1 - Konstantinidis, K. A1 - Kruger, H. A1 - Kurth, William S. A1 - Labrianidis, C. A1 - Lainey, V. A1 - Lamy, L. L. A1 - Laneuville, Matthieu A1 - Lucchesi, D. A1 - Luntzer, A. A1 - MacArthur, J. A1 - Maier, A. A1 - Masters, A. A1 - McKenna-Lawlor, S. A1 - Melin, H. A1 - Milillo, A. A1 - Moragas-Klostermeyer, Georg A1 - Morschhauser, Achim A1 - Moses, J. I. A1 - Mousis, O. A1 - Nettelmann, N. A1 - Neubauer, F. M. A1 - Nordheim, T. A1 - Noyelles, B. A1 - Orton, G. S. A1 - Owens, Mathew A1 - Peron, R. A1 - Plainaki, C. A1 - Postberg, F. A1 - Rambaux, N. A1 - Retherford, K. A1 - Reynaud, Serge A1 - Roussos, Elias A1 - Russell, C. T. A1 - Rymer, Am. A1 - Sallantin, R. A1 - Sanchez-Lavega, A. A1 - Santolik, O. A1 - Saur, J. A1 - Sayanagi, Km. A1 - Schenk, P. A1 - Schubert, J. A1 - Sergis, N. A1 - Sittler, E. C. A1 - Smith, A. A1 - Spahn, Frank A1 - Srama, Ralf A1 - Stallard, T. A1 - Sterken, V. A1 - Sternovsky, Zoltan A1 - Tiscareno, M. A1 - Tobie, G. A1 - Tosi, F. A1 - Trieloff, M. A1 - Turrini, D. A1 - Turtle, E. P. A1 - Vinatier, S. A1 - Wilson, R. A1 - Zarkat, P. T1 - The science case for an orbital mission to Uranus: Exploring the origins and evolution of ice giant planets JF - Planetary and space science N2 - Giant planets helped to shape the conditions we see in the Solar System today and they account for more than 99% of the mass of the Sun's planetary system. They can be subdivided into the Ice Giants (Uranus and Neptune) and the Gas Giants (Jupiter and Saturn), which differ from each other in a number of fundamental ways. Uranus, in particular is the most challenging to our understanding of planetary formation and evolution, with its large obliquity, low self-luminosity, highly asymmetrical internal field, and puzzling internal structure. Uranus also has a rich planetary system consisting of a system of inner natural satellites and complex ring system, five major natural icy satellites, a system of irregular moons with varied dynamical histories, and a highly asymmetrical magnetosphere. Voyager 2 is the only spacecraft to have explored Uranus, with a flyby in 1986, and no mission is currently planned to this enigmatic system. However, a mission to the uranian system would open a new window on the origin and evolution of the Solar System and would provide crucial information on a wide variety of physicochemical processes in our Solar System. These have clear implications for understanding exoplanetary systems. In this paper we describe the science case for an orbital mission to Uranus with an atmospheric entry probe to sample the composition and atmospheric physics in Uranus' atmosphere. The characteristics of such an orbiter and a strawman scientific payload are described and we discuss the technical challenges for such a mission. This paper is based on a white paper submitted to the European Space Agency's call for science themes for its large-class mission programme in 2013. KW - Uranus KW - Magnetosphere KW - Atmosphere KW - Natural satellites KW - Rings KW - Planetary interior Y1 - 2014 U6 - https://doi.org/10.1016/j.pss.2014.08.009 SN - 0032-0633 VL - 104 SP - 122 EP - 140 PB - Elsevier CY - Oxford ER - TY - JOUR A1 - Arthur, S. J. T1 - Wolf-Rayet nebulae and the wind-interstellar medium interaction JF - Wolf-Rayet Stars : Proceedings of an International Workshop held in Potsdam, Germany, 1.–5. June 2015 N2 - I review our current understanding of the interaction between a Wolf-Rayet star's fast wind and the surrounding medium, and discuss to what extent the predictions of numerical simulations coincide with multiwavelength observations of Wolf-Rayet nebulae. Through a series of examples, I illustrate how changing the input physics affects the results of the numerical simulations. Finally, I discuss how numerical simulations together with multiwavelength observations of these objects allow us to unpick the previous mass-loss history of massive stars. Y1 - 2015 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-88267 SP - 315 EP - 320 ER - TY - THES A1 - Arvind, Malavika T1 - Regarding the role of aggregation and structural order on the mechanism of molecular doping of semiconducting polymers T1 - Die Rolle von Aggregation und struktureller Ordnung auf den Mechanismus der molekularen Dotierung von halbleitenden Polymeren BT - from solutions to films BT - von Lösungen zu Filmen N2 - Polymeric semiconductors are strong contenders for replacing traditional inorganic semiconductors in electronic applications requiring low power, low cost and flexibility, such as biosensors, flexible solar cells and electronic displays. Molecular doping has the potential to enable this revolution by improving the conductivity and charge transport properties of this class of materials. Despite decades of research in this field, gaps in our understanding of the nature of dopant–polymer interactions has resulted in limited commercialization of this technology. This work aims at providing a deeper insight into the underlying mechanisms of molecular p-doping of semiconducting polymers in the solution and solid-state, and thereby bring the scientific community closer to realizing the dream of making organic semiconductors commonplace in the electronics industry. The role of 1) dopant size/shape, 2) polymer chain aggregation and 3) charge delocalization on the doping mechanism and efficiency is addressed using optical (UV-Vis-NIR) and electron paramagnetic resonance (EPR) spectroscopies. By conducting a comprehensive study of the nature and concentration of the doping-induced species in solutions of the polymer poly(3-hexylthiophene) (P3HT) with 3 different dopants, we identify the unique optical signatures of the delocalized polaron, localized polaron and charge-transfer complex, and report their extinction coefficient values. Furthermore, with X-ray diffraction, atomic force microscopy and electrical conductivity measurements, we study the impact of processing technique and doping mechanism on the morphology and thereby, charge transport through the doped films. This work demonstrates that the doping mechanism and type of doping-induced species formed are strongly influenced by the polymer backbone arrangement rather than dopant shape/size. The ability of the polymer chain to aggregate is found to be crucial for efficient charge transfer (ionization) and polaron delocalization. At the same time, our results suggest that the high ionization efficiency of a dopant–polymer system in solution may subsequently hinder efficient charge transport in the solid-state due to the reduction in the fraction of tie chains, which enable charges to move efficiently between aggregated domains in the films. This study demonstrates the complex multifaceted nature of polymer doping while providing important hints for the future design of dopant-host systems and film fabrication techniques. N2 - Polymer-Halbleiter sind vielversprechende Kandidaten für den Ersatz traditioneller anorganischer Halbleiter in elektronischen Anwendungen, die einen geringen Stromverbrauch, niedrige Kosten und mechanische Flexibilität erfordern, wie z.B. Biosensoren, flexible Solarzellen und elektronische Bildschirme. Molekulare Dotierung hat das Potenzial, diese Revolution zu ermöglichen, indem sie die Leitfähigkeit und die Ladungstransporteigenschaften dieser Materialklasse verbessert. Trotz jahrzehntelanger Forschung auf diesem Gebiet hat das unvollständige Verständnis der Dotierstoff-Polymer-Wechselwirkungen nur zu einer begrenzten Kommerzialisierung dieser Technologie geführt.Ziel dieser Arbeit ist es, einen tieferen Einblick in die zugrunde liegenden Mechanismen der molekularen p-Dotierung von halbleitenden Polymeren in Lösung und im festen Zustand zu geben und dadurch die wissenschaftliche Gemeinschaft näher an die Verwirklichung des Traums heran zu bringen, organische Halbleiter in der Elektronikindustrie alltäglich zu machen. Diese Arbeit zeigt, dass der Dotierungsmechanismus und die Art der gebildeten, dotierungsinduzierten Spezies eher durch die Anordnung des Polymerrückgrats als durch die Form/Größe des Dotierstoffs beeinflusst werden. Die Fähigkeit der Polymerkette, zu aggregieren, stellt sich als entscheidend für einen effizienten Ladungstransfer (d.h. Ionisierung) und die Polaron-Delokalisierung heraus. Gleichzeitig deuten unsere Ergebnisse darauf hin, dass die hohe Ionisationseffizienz eines Dotierstoff-Polymersystems in der Lösung eine Beinträchtigung des effizienten Ladungstransport im festen Zustand nach sich ziehen kann, da der Anteil der Verbindungsketten, die eine effiziente Bewegung von Ladungen zwischen aggregierten Domänen in dünnen Filmen ermöglichen, reduziert wird. Diese Arbeit verdeutlicht die komplexe, vielschichtige Natur der Polymerdotierung und gibt dabei wichtige Hinweise für das zukünftige Design von Dotierstoff-Wirtssystemen und Filmherstellungstechniken. KW - molecular doping KW - organic semiconductors KW - Lewis acid doping KW - optical spectroscopy KW - thin films KW - semiconducting polymer KW - conductivity KW - dip doping KW - polymer aggregation KW - Dotierung KW - Polymer-Halbleiter KW - Leitfähigkeit KW - Lewis-Säure Dotierung KW - organische Halbleiter KW - Polymeraggregation KW - halbleitendes Polymer KW - Dünn film KW - optische Spektroskopie KW - molekulare Dotierung KW - Dip-Dotierung Y1 - 2021 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-500606 ER - TY - THES A1 - Arya, Pooja T1 - Light controlled active and passive motion of colloidal particles N2 - In this dissertation we introduce a concept of light driven active and passive manipulation of colloids trapped at solid/liquid interface. The motion is induced due to generation of light driven diffusioosmotic flow (LDDO) upon irradiation with light of appropriate wavelength. The origin of the flow is due to osmotic pressure gradient resulting from a concentration gradient at the solid/liquid interface of the photosensitive surfactant present in colloidal dispersion. The photosensitive surfactant consists of a cationic head group and a hydrophobic tail in which azobenzene group is integrated in. The azobenzene is known to undergo reversible photo-isomerization from a stable trans to a meta stable cis state under irradiation with UV light. Exposure to light of larger wavelength results in back photo-isomerization from cis to trans state. The two isomers have different molecular properties, for instance, trans isomer has a rod like structure and low polarity (0 dipole moment), whereas cis one is bent and has a dipole moment of ~3 Debye. Being integrated in the hydrophobic tail of the surfactant molecule, the azobenzene state determines the hydrophobicity of the whole molecule: in the trans state the surfactant is more hydrophobic than in the cis-state. In this way many properties of the surfactant such as the CMC, solubility and the interaction potential with a solid surface can be altered by light. When the solution containing such a surfactant is irradiated with focused light, a concentration gradient of different isomers is formed near the boundary of the irradiated area near the solid surface resulting in osmotic pressure gradient. The generated diffusioosmotic (DO) flow carries the particles passively along. The local-LDDO flow can be generated around and by each particle when mesoporous silica colloids are dispersed in the surfactant solution. This is because porous particles act as a sink/source which absorbs azobenzene molecule in trans state and expels it when it is in the cis state. The DO flows generated at each particle interact resulting in aggregation or separation depending upon the initial state of surfactant molecules. The kinetic of aggregation and separation can be controlled and manipulated by altering the parameters such as the wavelength and intensity of the applied light, as well as surfactant and particle concentration. Using two wavelengths simultaneously allows for dynamic gathering and separation creating fascinating patterns such as 2D disk of well separated particles or establishing collective complex behaviour of particle ensemble as described in this thesis. The mechanism of l-LDDO is also used to generate self-propelled motion. This is possible when half of the porous particle is covered by metal layer, basically blocking the pores on one side. The LDDO flow generated on uncapped side pushes the particle forward resulting in a super diffusive motion. The system of porous particle and azobenzene containing surfactant molecule can be utilized for various application such as drug delivery, cargo transportation, self-assembling, micro motors/ machines or micro patterning. N2 - In dieser Doktorarbeit führen wir das Konzept der lichtinduzierten Diffusioosmose (LDDO) zur licht-kontrollierten passiven und aktiven Bewegung von Kolloiden an der fest-flüssig Grenzfläche ein. Bei diesem neuartigen Phänomen wird ein Grenzflächenfluss mittels Lichtes bestimmter Wellenlänge erzeugt. Ein lichtempfindliches Tensid wirkt hierbei als Quelle der Diffusioosmose: Durch Einstrahlung von Licht wird ein Konzentrationsgradient an der Oberfläche erzeugt, der wiederum ein Ungleichgewicht im lateralen osmotischen Druck verursacht. Dieser Druckunterschied führt dann zu einem grenzflächennahen diffusioosmotischen Fluss. Das lichtaktive Molekül besteht aus einer kationischen Kopfgruppe und einer hydrophoben Kohlenstoffkette, in die die Azobenzolgruppe eingebettet ist. Azobenzol fungiert hier als Lichtschalter, da es mit Licht zwischen einem stabilen trans und einem metastabilen cis Zustand hin- und hergeschaltet werden kann. Nahes UV Licht führt hier zur trans-cis und sichtbares Licht zur cis-trans Isomerisation. Das trans Isomer unterscheidet sich in einigen Eigenschaften vom cis Isomer. So ist z.B. das trans-Isomer langgestreckt und besitzt eine geringe Polarität (verschwindendes Dipolmoment), währenddessen das cis Isomer gebogen ist und ein deutliches Dipolmoment von ca. 3 Debye besitzt. Durch die Integration der Azobenzolgruppe in die hydrophobe Kette des Tensids, bestimmt der Isomerisationszustand des Tensids die Hydrophobizität des gesamten Moleküls: Der trans Zustand ist deutlich hydrophober als der cis Zustand. Dieser Unterschied zeigt sich in den Löslichkeitseigenschaften des Moleküls, der kritischen Mizellenkonzentration sowie des Wechselwirkungspotentials zwischen Molekül und Grenzfläche. Dies kann genutzt werden, um diese Eigenschaften mittels Lichtbestrahlung zu ändern. Wird das Molekül in Wasser gelöst und mit fokussiertem Licht bestrahlt, kann ein isomerer Konzentrationsgradient im Bestrahlungsbereich an der fest-flüssig Grenzfläche erzeugt werden, der wiederum in einem osmotischen Druckgunterschied resultiert. Die daraus resultierende Diffusioosmose (DO), welche an der Grenzfläche erzeugt wird, ist in der Lage Kolloide, die sich an der Grenzfläche befinden, transportieren (passiv). Im Unterschied dazu kann ein sogenannter lokaler diffusioosmotischer Fluss (l-LDDO) um jedes einzelne Kolloid erzeugt werden, sobald es sich um meso-poröse Kolloide handelt. Hierbei agiert jedes Kolloid selbst als Konzentrationsquelle- bzw. –senke (ähnlich dem fokussiertem Licht im oberen Fall). Je nach Isomerisationszustand lagert sich das Molekül eher im Kolloid an oder bevorzugt die Umgebung des Wassers. Befindet sich das Molekül im trans Zustand lagert es sich im Kolloid an, während es im cis Zustand eher die Umgebung des Wassers sucht. Der diffusioosmotische Fluss wird um jedes einzelne Kolloid erzeugt, wodurch eine Wechselwirkung zwischen allen Kolloiden zustande kommt, die entweder anziehend oder abstoßend sein kann. Das hängt vom Isomerisationszustand der Tensidmoleküle vor der Bestrahlung ab. Durch die Änderung der folgenden Parameter kann die Bewegung der Kolloide kontrolliert werden: Lichtwellenlänge, Lichtintensität, Tensidkonzentration, Kolloidkonzentration. Durch die gleichzeitige Verwendung zweier verschiedener Lichtquellen (mit unterschiedlichen Wellenlängen), ist es möglich eine interessante Dynamik in der Anziehung und Abstoßung der Kolloide zu erzeugen, die faszinierende Kolloidformationen entstehen lassen wie sie in dieser Arbeit näher beschrieben werden. Das Phänomen der lokalen Diffusioosmose kann auch zu selbst-getriebener Bewegung führen, nämlich wenn eine Hälfte des Kolloids bedeckt wird (z.B. mit einer Metallschicht) und somit für Tensidmoleküle undurchlässig macht. Der diffusioosmotische Fluss, der auf der unbedeckten Seite des Kolloids erzeugt wird, bewegt das Kolloid in eine Richtung fort und führt so durch Überlagerung zur thermischen Bewegung zu super-diffusivem Verhalten. Das System, bestehend aus porösen Kolloiden und azobenzolhaltigem Tensidmolekül kann sinnführend genutzt werden, z.B. für folgende Anwendungen: gezieltem Medikamententransport, Mikrofrachttransport, Selbstassemblierung, Mikromotoren/-maschinen oder Mikrostrukturierung. T2 - Licht-kontrollierten passive und aktive Bewegung kolloidaler Partikel KW - Azobenzene containing surfactant KW - Photochemistry KW - Porous silica particles KW - Janus colloids KW - LDDO KW - diffusioosmotic flow KW - Hydrophobic and hydrophillic interactions KW - Kinetics of photoisomerization KW - Azobenzol enthaltendes Tensid KW - hydrophoben und hydrophile Wechselwirkungen KW - Janus-Kolloid KW - LDDO KW - Photochemie KW - poröse Siliciumdioxidpartikel KW - diffusioosmotischer Fluss KW - Isomerisierung Kinetik Y1 - 2020 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-483880 ER - TY - JOUR A1 - Arya, Pooja A1 - Feldmann, David A1 - Kopyshev, Alexey A1 - Lomadze, Nino A1 - Santer, Svetlana T1 - Light driven guided and self-organized motion of mesoporous colloidal particles JF - Soft matter N2 - We report on guided and self-organized motion of ensembles of mesoporous colloidal particles that can undergo dynamic aggregation or separation upon exposure to light. The forces on particles involve the phenomenon of light-driven diffusioosmosis (LDDO) and are hydrodynamic in nature. They can be made to act passively on the ensemble as a whole but also used to establish a mutual interaction between particles. The latter scenario requires a porous colloid morphology such that the particle can act as a source or sink of a photosensitive surfactant, which drives the LDDO process. The interplay between the two modes of operation leads to fascinating possibilities of dynamical organization and manipulation of colloidal ensembles adsorbed at solid-liquid interfaces. While the passive mode can be thought of to allow for a coarse structuring of a cloud of colloids, the inter-particle mode may be used to impose a fine structure on a 2D particle grid. Local flow is used to impose and tailor interparticle interactions allowing for much larger interaction distances that can be achieved with, e.g., DLVO type of forces, and is much more versatile. Y1 - 2019 U6 - https://doi.org/10.1039/c9sm02068c SN - 1744-683X SN - 1744-6848 VL - 16 IS - 5 SP - 1148 EP - 1155 PB - Royal Society of Chemistry CY - Cambridge ER - TY - JOUR A1 - Arya, Pooja A1 - Jelken, Joachim A1 - Feldmann, David A1 - Lomadze, Nino A1 - Santer, Svetlana T1 - Light driven diffusioosmotic repulsion and attraction of colloidal particles JF - The journal of chemical physics : bridges a gap between journals of physics and journals of chemistr N2 - In this paper, we introduce the phenomenon of light driven diffusioosmotic long-range attraction and repulsion of porous particles under irradiation with UV light. The change in the inter-particle interaction potential is governed by flow patterns generated around single colloids and results in reversible aggregation or separation of the mesoporous silica particles that are trapped at a solid surface. The range of the interaction potential extends to several times the diameter of the particle and can be adjusted by varying the light intensity. The "fuel" of the process is a photosensitive surfactant undergoing photo-isomerization from a more hydrophobic trans-state to a rather hydrophilic cis-state. The surfactant has different adsorption affinities to the particles depending on the isomerization state. The trans-isomer, for example, tends to accumulate in the negatively charged pores of the particles, while the cis-isomer prefers to remain in the solution. This implies that when under UV irradiation cis-isomers are being formed within the pores, they tend to diffuse out readily and generate an excess concentration near the colloid's outer surface, ultimately resulting in the initiation of diffusioosmotic flow. The direction of the flow depends strongly on the dynamic redistribution of the fraction of trans- and cis-isomers near the colloids due to different kinetics of photo-isomerization within the pores as compared to the bulk. The unique feature of the mechanism discussed in the paper is that the long-range mutual repulsion but also the attraction can be tuned by convenient external optical stimuli such as intensity so that a broad variety of experimental situations for manipulation of a particle ensemble can be realized. Y1 - 2020 U6 - https://doi.org/10.1063/5.0007556 SN - 0021-9606 SN - 1089-7690 VL - 152 IS - 19 PB - American Institute of Physics CY - Melville, NY ER - TY - JOUR A1 - Arya, Pooja A1 - Jelken, Joachim A1 - Lomadze, Nino A1 - Santer, Svetlana A1 - Bekir, Marek T1 - Kinetics of photo-isomerization of azobenzene containing surfactants JF - The journal of chemical physics : bridges a gap between journals of physics and journals of chemistry N2 - We report on photoisomerization kinetics of azobenzene containing surfactants in aqueous solution. The surfactant molecule consists of a positively charged trimethylammonium bromide head group, a hydrophobic spacer connecting via 6 to 10 CH2 groups to the azobenzene unit, and the hydrophobic tail of 1 and 3CH(2) groups. Under exposure to light, the azobenzene photoisomerizes from more stable trans- to metastable cis-state, which can be switched back either thermally in dark or by illumination with light of a longer wavelength. The surfactant isomerization is described by a kinetic model of a pseudo first order reaction approaching equilibrium, where the intensity controls the rate of isomerization until the equilibrated state. The rate constants of the trans-cis and cis-trans photoisomerization are calculated as a function of several parameters such as wavelength and intensity of light, the surfactant concentration, and the length of the hydrophobic tail. The thermal relaxation rate from cis- to trans-state is studied as well. The surfactant isomerization shows a different kinetic below and above the critical micellar concentration of the trans isomer due to steric hindrance within the densely packed micelle but does not depend on the spacer length. KW - genomic DNA conformation KW - water-interface KW - light photocontrol KW - driven KW - manipulation KW - photoisomerization KW - molecules Y1 - 2020 U6 - https://doi.org/10.1063/1.5135913 SN - 0021-9606 SN - 1089-7690 VL - 152 IS - 2 PB - American Institute of Physics CY - Melville ER - TY - JOUR A1 - Asawapirom, Udom A1 - Bulut, F. A1 - Farrell, Tony A1 - Gadermaier, C. A1 - Gamerith, S. A1 - Güntner, Roland A1 - Kietzke, Thomas A1 - Patil, S. A1 - Piok, T. A1 - Montenegro, Rivelino V. D. A1 - Stiller, Burkhard A1 - Tiersch, Brigitte A1 - Landfester, Katharina A1 - List, E. J. W. A1 - Neher, Dieter A1 - Torres, C. S. A1 - Scherf, Ullrich T1 - Materials for polymer electronics applications semiconducting polymer thin films and nanoparticles N2 - The paper presents two different approaches to nanostructured semiconducting polymer materials: (i) the generation of aqueous semiconducting polymer dispersions (semiconducting polymer nanospheres SPNs) and their processing into dense films and layers, and (ii) the synthesis of novel semiconducting polyfluorene-block-polyaniline (PF-b-PANI) block copolymers composed of conjugated blocks of different redox potentials which form nanosized morphologies in the solid state Y1 - 2004 SN - 1022-1360 ER - TY - THES A1 - Aseev, Nikita T1 - Modeling and understanding dynamics of charged particles in the Earth's inner magnetosphere T1 - Modellierung und Untersuchung der Dynamik geladener Teilchen in der inneren Magnetosphäre der Erde N2 - The Earth's inner magnetosphere is a very dynamic system, mostly driven by the external solar wind forcing exerted upon the magnetic field of our planet. Disturbances in the solar wind, such as coronal mass ejections and co-rotating interaction regions, cause geomagnetic storms, which lead to prominent changes in charged particle populations of the inner magnetosphere - the plasmasphere, ring current, and radiation belts. Satellites operating in the regions of elevated energetic and relativistic electron fluxes can be damaged by deep dielectric or surface charging during severe space weather events. Predicting the dynamics of the charged particles and mitigating their effects on the infrastructure is of particular importance, due to our increasing reliance on space technologies. The dynamics of particles in the plasmasphere, ring current, and radiation belts are strongly coupled by means of collisions and collisionless interactions with electromagnetic fields induced by the motion of charged particles. Multidimensional numerical models simplify the treatment of transport, acceleration, and loss processes of these particles, and allow us to predict how the near-Earth space environment responds to solar storms. The models inevitably rely on a number of simplifications and assumptions that affect model accuracy and complicate the interpretation of the results. In this dissertation, we quantify the processes that control electron dynamics in the inner magnetosphere, paying particular attention to the uncertainties of the employed numerical codes and tools. We use a set of convenient analytical solutions for advection and diffusion equations to test the accuracy and stability of the four-dimensional Versatile Electron Radiation Belt (VERB-4D) code. We show that numerical schemes implemented in the code converge to the analytical solutions and that the VERB-4D code demonstrates stable behavior independent of the assumed time step. The order of the numerical scheme for the convection equation is demonstrated to affect results of ring current and radiation belt simulations, and it is crucially important to use high-order numerical schemes to decrease numerical errors in the model. Using the thoroughly tested VERB-4D code, we model the dynamics of the ring current electrons during the 17 March 2013 storm. The discrepancies between the model and observations above 4.5 Earth's radii can be explained by uncertainties in the outer boundary conditions. Simulation results indicate that the electrons were transported from the geostationary orbit towards the Earth by the global-scale electric and magnetic fields. We investigate how simulation results depend on the input models and parameters. The model is shown to be particularly sensitive to the global electric field and electron lifetimes below 4.5 Earth's radii. The effects of radial diffusion and subauroral polarization streams are also quantified. We developed a data-assimilative code that blends together a convection model of energetic electron transport and loss and Van Allen Probes satellite data by means of the Kalman filter. We show that the Kalman filter can correct model uncertainties in the convection electric field, electron lifetimes, and boundary conditions. It is also demonstrated how the innovation vector - the difference between observations and model prediction - can be used to identify physical processes missing in the model of energetic electron dynamics. We computed radial profiles of phase space density of ultrarelativistic electrons, using Van Allen Probes measurements. We analyze the shape of the profiles during geomagnetically quiet and disturbed times and show that the formation of new local minimums in the radial profiles coincides with the ground observations of electromagnetic ion-cyclotron (EMIC) waves. This correlation indicates that EMIC waves are responsible for the loss of ultrarelativistic electrons from the heart of the outer radiation belt into the Earth's atmosphere. N2 - Die innere Magnetosphäre der Erde ist ein sehr dynamisches System, das hauptsächlich vom äußeren Sonnenwind beeinflusst wird, der auf das Magnetfeld unseres Planeten einwirkt. Störungen im Sonnenwind, wie z.B. koronale Massenauswürfe und sogenannte Korotierende Wechselwirkungsbereiche, verursachen geomagnetische Stürme, die zu deutlichen Veränderungen der Populationen geladener Teilchen in der inneren Magnetosphäre führen - Plasmasphäre, Ringstrom und Strahlungsgürtel. Satelliten, die in Regionen mit erhöhten energetischen und relativistischen Elektronenflüssen betrieben werden, können durch tiefe dielektrische Ladung oder Oberflächenladungen bei schweren Weltraumwetterereignissen beschädigt werden. Die Vorhersage der Dynamik der geladenen Teilchen und die Abschwächung ihrer Auswirkungen auf die Infrastruktur sind heutzutage von besonderer Bedeutung, insbesondere aufgrund unserer zunehmenden Abhängigkeit von Weltraumtechnologien. Die Dynamik von Teilchen in der Plasmasphäre, des Ringstrom und in den Strahlungsgürteln sind durch Kollisionen und kollisionsfreie Wechselwirkungen mit elektromagnetischen Feldern, die durch die Bewegung geladener Teilchen induziert werden, stark gekoppelt. Mehrdimensionale numerische Modelle vereinfachen die Betrachtung von Transport-, Beschleunigungs- und Verlustprozessen dieser Partikel und ermöglichen es uns, vorherzusagen, wie die erdnahe Weltraumumgebung auf Sonnenstürme reagiert. Die Modelle beruhen zwangsläufig auf einer Reihe von Vereinfachungen und Voraussetzungen, die sich auf die Modellgenauigkeit auswirken und die Interpretation der Ergebnisse erschweren. In dieser Dissertation quantifizieren wir die Prozesse, die die Dynamik der Elektronen in der inneren Magnetosphäre steuern. Dabei richten wir den Fokus insbesondere auch auf die Unsicherheiten der verwendeten numerischen Codes. Wir verwenden eine Reihe praktischer analytischer Lösungen für Advektions- und Diffusionsgleichungen, um die Genauigkeit und Stabilität des 4-dimensionalen ''Versatile Electron Radiation Belt'' Codes (VERB-4D Code) zu testen. Wir zeigen, dass die im Code implementierten numerischen Schemata zu den analytischen Lösungen konvergieren und der Code sich unabhängig vom angenommenen Zeitschritt stabil verhält. Wir demonstrieren, wie die Genauigkeit des numerischen Schemas für die Konvektionsgleichung die Ergebnisse von Ringstrom- und Strahlungsgürtelsimulationen beeinflussen kann, und dass es von entscheidender Beteutung ist, numerische Schemata höherer Ordnung zu verwenden, um numerische Fehler im Modell zu reduzieren. Mit dem ausführlich getesteten VERB-4D Code modellieren wir die Dynamik der Ringstromelektronen während des Sturms vom 17. März 2013. Wir zeigen, dass die Diskrepanzen zwischen dem Modell und Beobachtungen oberhalb von 4.5 Erdradien durch Unsicherheiten in den äußeren Randbedingungen erklärt werden können und dass die Elektronen durch die globalen elektrischen und magnetischen Felder von der geostationäre Umlaufbahn zur Erde transportiert wurden. Wir untersuchen weiterhin, wie die Simulationsergebnisse von den Eingabemodellen und Parametern abhängen. Wir zeigen, dass das Modell besonders empfindlich für das globale elektrische Feld und die Lebensdauer der Elektronen unterhalb von 4.5 Erdradien ist. Außerdem quantifizieren wir auch die Auswirkungen von radialer Diffusion und subauroralen Polarisationsströmen. Wir haben einen datenassimilativen Code entwickelt, der mithilfe des Kalman-Filters ein Konvektionsmodell für den Transport und den Verlust energetischer Elektronen mit den Satellitendaten der Van Allen Probes kombiniert. Wir zeigen, dass die Verwendung eines Kalman-Filters Modellunsicherheiten im elektrischen Konvektionsfeld, in der Lebensdauer der Elektronen und in den Randbedingungen korrigieren kann. Weiterhin zeigen wir, wie der Innovationsvektor - die Differenz zwischen Beobachtungen und Modellvorhersagen - verwendet werden kann, um physikalische Prozesse zu identifizieren, die im Modell der Dynamik der energetischen Elektronen fehlen. Außerdem berechnen wir radiale Profile der Phasenraumdichte ultrarelativistischer Elektronen mithilfe von Van Allen Probes-Messungen. Wir analysieren die Form der Profile und zeigen, dass die Entstehung neuer lokaler Minima in den radialen Profilen mit den Bodenbeobachtungen von EMIC-Wellen übereinstimmt. Diese Korrelation legt nahe, dass EMIC-Wellen für den Verlust ultrarelativistischer Elektronen vom Herzen des äußeren Strahlungsgürtels in die Erdatmosphäre verantwortlich sind. KW - ring current electrons KW - radiation belts KW - mathematical modeling KW - wave-particle interactions KW - data assimilation KW - Ringstromelektronen KW - Strahlungsgürtel KW - mathematische Modellierung KW - Wellen-Teilchen Wechselwirkungen KW - Datenassimilation Y1 - 2020 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-479211 ER - TY - JOUR A1 - Aseev, Nikita A1 - Shprits, Yuri Y. T1 - Reanalysis of ring current electron phase space densities using van allen probe observations, convection model, and log‐normal kalman filter JF - Space weather : the international journal of research and applications N2 - Models of ring current electron dynamics unavoidably contain uncertainties in boundary conditions, electric and magnetic fields, electron scattering rates, and plasmapause location. Model errors can accumulate with time and result in significant deviations of model predictions from observations. Data assimilation offers useful tools which can combine physics-based models and measurements to improve model predictions. In this study, we systematically analyze performance of the Kalman filter applied to a log-transformed convection model of ring current electrons and Van Allen Probe data. We consider long-term dynamics of mu = 2.3 MeV/G and K = 0.3 G(1/2) R-E electrons from 1 February 2013 to 16 June 2013. By using synthetic data, we show that the Kalman filter is capable of correcting errors in model predictions associated with uncertainties in electron lifetimes, boundary conditions, and convection electric fields. We demonstrate that reanalysis retains features which cannot be fully reproduced by the convection model such as storm-time earthward propagation of the electrons down to 2.5 R-E. The Kalman filter can adjust model predictions to satellite measurements even in regions where data are not available. We show that the Kalman filter can adjust model predictions in accordance with observations for mu = 0.1, 2.3, and 9.9 MeV/G and constant K = 0.3 G(1/2) R-E electrons. The results of this study demonstrate that data assimilation can improve performance of ring current models, better quantify model uncertainties, and help deeper understand the physics of the ring current particles. Y1 - 2019 U6 - https://doi.org/10.1029/2018SW002110 SN - 1542-7390 VL - 17 IS - 4 SP - 619 EP - 638 PB - American Geophysical Union CY - Washington ER - TY - JOUR A1 - Aseev, Nikita A1 - Shprits, Yuri Y. A1 - Drozdov, Alexander A1 - Kellerman, Adam C. T1 - Numerical applications of the advective-diffusive codes for the inner magnetosphere JF - Space Weather: The International Journal of Research and Applications N2 - In this study we present analytical solutions for convection and diffusion equations. We gather here the analytical solutions for the one-dimensional convection equation, the two-dimensional convection problem, and the one- and two-dimensional diffusion equations. Using obtained analytical solutions, we test the four-dimensional Versatile Electron Radiation Belt code (the VERB-4D code), which solves the modified Fokker-Planck equation with additional convection terms. The ninth-order upwind numerical scheme for the one-dimensional convection equation shows much more accurate results than the results obtained with the third-order scheme. The universal limiter eliminates unphysical oscillations generated by high-order linear upwind schemes. Decrease in the space step leads to convergence of a numerical solution of the two-dimensional diffusion equation with mixed terms to the analytical solution. We compare the results of the third- and ninth-order schemes applied to magnetospheric convection modeling. The results show significant differences in electron fluxes near geostationary orbit when different numerical schemes are used. KW - advective-diffusive codes KW - inner magnetosphere KW - numerical schemes Y1 - 2016 U6 - https://doi.org/10.1002/2016SW001484 SN - 1542-7390 VL - 14 SP - 993 EP - 1010 PB - American Geophysical Union CY - Washington ER - TY - JOUR A1 - Aseev, Nikita A1 - Shprits, Yuri Y. A1 - Drozdov, Alexander A1 - Kellerman, Adam C. A1 - Usanova, Maria E. A1 - Wang, D. A1 - Zhelavskaya, Irina T1 - Signatures of Ultrarelativistic Electron Loss in the Heart of the Outer Radiation Belt Measured by Van Allen Probes JF - Journal of geophysical research : Space physics N2 - Up until recently, signatures of the ultrarelativistic electron loss driven by electromagnetic ion cyclotron (EMIC) waves in the Earth's outer radiation belt have been limited to direct or indirect measurements of electron precipitation or the narrowing of normalized pitch angle distributions in the heart of the belt. In this study, we demonstrate additional observational evidence of ultrarelativistic electron loss that can be driven by resonant interaction with EMIC waves. We analyzed the profiles derived from Van Allen Probe particle data as a function of time and three adiabatic invariants between 9 October and 29 November 2012. New local minimums in the profiles are accompanied by the narrowing of normalized pitch angle distributions and ground‐based detection of EMIC waves. Such a correlation may be indicative of ultrarelativistic electron precipitation into the Earth's atmosphere caused by resonance with EMIC waves. Y1 - 2017 U6 - https://doi.org/10.1002/2017JA024485 SN - 2169-9380 SN - 2169-9402 VL - 122 SP - 10102 EP - 10111 PB - American Geophysical Union CY - Washington ER - TY - JOUR A1 - Asghari, N. A1 - Broeg, C. A1 - Carone, L. A1 - Casas-Miranda, R. A1 - Palacio, J. C. C. A1 - Csillik, I. A1 - Dvorak, R. A1 - Freistetter, F. A1 - Hadjivantsides, G. A1 - Hussmann, H. A1 - Khramova, A. A1 - Khristoforova, M. A1 - Khromova, I. A1 - Kitiashivilli, I. A1 - Kozlowski, S. A1 - Laakso, T. A1 - Laczkowski, T. A1 - Lytvinenko, D. A1 - Miloni, O. A1 - Morishima, R. A1 - Moro-Martin, A. A1 - Paksyutov, V. A1 - Pal, A. A1 - Patidar, V. A1 - Pecnik, B. A1 - Peles, O. A1 - Pyo, J. A1 - Quinn, T. A1 - Rodriguez, A. A1 - Romano, C. A1 - Saikia, E. A1 - Stadel, J. A1 - Thiel, M. A1 - Todorovic, N. A1 - Veras, D. A1 - Neto, E. V. A1 - Vilagi, J. A1 - von Bloh, Werner A1 - Zechner, R. A1 - Zhuchkova, E. T1 - Stability of terrestrial planets in the habitable zone of G1 777 A, HD 72659, G1 614, 47 Uma and HD 4208 N2 - We have undertaken a thorough dynamical investigation of five extrasolar planetary systems using extensive numerical experiments. The systems Gl 777 A, HD 72659, Gl 614, 47 Uma and HD 4208 were examined concerning the question of whether they could host terrestrial-like planets in their habitable zones (HZ). First we investigated the mean motion resonances between fictitious terrestrial planets and the existing gas giants in these five extrasolar systems. Then a fine grid of initial conditions for a potential terrestrial planet within the HZ was chosen for each system, from which the stability of orbits was then assessed by direct integrations over a time interval of 1 million years. For each of the five systems the 2-dimensional grid of initial conditions contained 80 eccentricity points for the Jovian planet and up to 160 semimajor axis points for the fictitious planet. The computations were carried out using a Lie-series integration method with an adaptive step size control. This integration method achieves machine precision accuracy in a highly efficient and robust way, requiring no special adjustments when the orbits have large eccentricities. The stability of orbits was examined with a determination of the Renyi entropy, estimated from recurrence plots, and with a more straightforward method based on the maximum eccentricity achieved by the planet over the 1 million year integration. Additionally, the eccentricity is an indication of the habitability of a terrestrial planet in the HZ; any value of e > 0.2 produces a significant temperature difference on a planet's surface between apoapse and periapse. The results for possible stable orbits for terrestrial planets in habitable zones for the five systems are: for Gl 777 A nearly the entire HZ is stable, for 47 Uma, HD 72659 and HD 4208 terrestrial planets can survive for a sufficiently long time, while for Gl 614 our results exclude terrestrial planets moving in stable orbits within the HZ. Studies such as this one are of primary interest to future space missions dedicated to finding habitable terrestrial planets in other stellar systems. Assessing the likelihood of other habitable planets, and more generally the possibility of other life, is the central question of astrobiology today. Our investigation indicates that, from the dynamical point of view, habitable terrestrial planets seem to be compatible with many of the currently discovered extrasolar systems Y1 - 2004 UR - http://www.aanda.org/ U6 - https://doi.org/10.1051/0004-6361:20040390 SN - 0004-6361 ER - TY - JOUR A1 - Ashton, Gregory A1 - Dietrich, Tim T1 - The use of hypermodels to understand binary neutron star collisions JF - Nature astronomy N2 - Gravitational waves from the collision of binary neutron stars provide a unique opportunity to study the behaviour of supranuclear matter, the fundamental properties of gravity and the cosmic history of our Universe. However, given the complexity of Einstein's field equations, theoretical models that enable source-property inference suffer from systematic uncertainties due to simplifying assumptions. We develop a hypermodel approach to compare and measure the uncertainty of gravitational-wave approximants. Using state-of-the-art models, we apply this new technique to the binary neutron star observations GW170817 and GW190425 and to the sub-threshold candidate GW200311_103121. Our analysis reveals subtle systematic differences (with Bayesian odds of similar to 2) between waveform models. A frequency-dependence study suggests that this may be due to the treatment of the tidal sector. This new technique provides a proving ground for model development and a means to identify waveform systematics in future observing runs where detector improvements will increase the number and clarity of binary neutron star collisions we observe. Y1 - 2022 U6 - https://doi.org/10.1038/s41550-022-01707-x SN - 2397-3366 VL - 6 IS - 8 SP - 961 EP - 967 PB - Nature portfolio CY - Berlin ER - TY - JOUR A1 - Assagra, Yuri A.O. A1 - Altafim, Ruy Alberto Pisani A1 - do Carmo, Joao P. A1 - Altafim, Ruy A.C. A1 - Rychkov, Dmitry A1 - Wirges, Werner A1 - Gerhard, Reimund T1 - A new route to piezo-polymer transducers: 3D printing of polypropylene ferroelectrets JF - IEEE transactions on dielectrics and electrical insulation N2 - Here, a promising approach for producing piezo-polymer transducers in a one-step process is presented. Using 3D-printing technology and polypropylene (PP) filaments, we are able to print a two-layered film structure with regular cavities of precisely controlled size and shape. It is found that the 3D-printed samples exhibit piezoelectric coefficients up to 200 pC/N, similar to those of other PP ferroelectrets, and their temporal and thermal behavior is in good agreement with those known of PP ferroelectrets. The piezoelectric response strongly decreases for applied pressures above 20 kPa, as the pressure in the air-filled cavities strongly influences the overall elastic modulus of ferroelectrets. KW - 3D printing KW - polymer ferroelectrets KW - sensors and actuators KW - piezoelectrets KW - electret polymers KW - soft electro-active materials KW - functional materials KW - soft matter Y1 - 2020 U6 - https://doi.org/10.1109/TDEI.2020.008461 SN - 1070-9878 SN - 1558-4135 VL - 27 IS - 5 SP - 1668 EP - 1674 PB - Inst. of Electr. and Electronics Engineers CY - Piscataway 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 - THES A1 - Ata, Metin T1 - Phase-space reconstructions of cosmic velocities and the cosmic web T1 - Phasenraumrekonstruktionen kosmischer Geschwindigkeiten und des kosmischen Netzes BT - structure formation models - galaxy bias models - galaxy redshift surveys - inference analysis N2 - In the current paradigm of cosmology, the formation of large-scale structures is mainly driven by non-radiating dark matter, making up the dominant part of the matter budget of the Universe. Cosmological observations however, rely on the detection of luminous galaxies, which are biased tracers of the underlying dark matter. In this thesis I present cosmological reconstructions of both, the dark matter density field that forms the cosmic web, and cosmic velocities, for which both aspects of my work are delved into, the theoretical formalism and the results of its applications to cosmological simulations and also to a galaxy redshift survey.The foundation of our method is relying on a statistical approach, in which a given galaxy catalogue is interpreted as a biased realization of the underlying dark matter density field. The inference is computationally performed on a mesh grid by sampling from a probability density function, which describes the joint posterior distribution of matter density and the three dimensional velocity field. The statistical background of our method is described in Chapter ”Implementation of argo”, where the introduction in sampling methods is given, paying special attention to Markov Chain Monte-Carlo techniques. In Chapter ”Phase-Space Reconstructions with N-body Simulations”, I introduce and implement a novel biasing scheme to relate the galaxy number density to the underlying dark matter, which I decompose into a deterministic part, described by a non-linear and scale-dependent analytic expression, and a stochastic part, by presenting a negative binomial (NB) likelihood function that models deviations from Poissonity. Both bias components had already been studied theoretically, but were so far never tested in a reconstruction algorithm. I test these new contributions againstN-body simulations to quantify improvements and show that, compared to state-of-the-art methods, the stochastic bias is inevitable at wave numbers of k≥0.15h Mpc^−1 in the power spectrum in order to obtain unbiased results from the reconstructions. In the second part of Chapter ”Phase-Space Reconstructions with N-body Simulations” I describe and validate our approach to infer the three dimensional cosmic velocity field jointly with the dark matter density. I use linear perturbation theory for the large-scale bulk flows and a dispersion term to model virialized galaxy motions, showing that our method is accurately recovering the real-space positions of the redshift-space distorted galaxies. I analyze the results with the isotropic and also the two-dimensional power spectrum.Finally, in Chapter ”Phase-space Reconstructions with Galaxy Redshift Surveys”, I show how I combine all findings and results and apply the method to the CMASS (for Constant (stellar) Mass) galaxy catalogue of the Baryon Oscillation Spectroscopic Survey (BOSS). I describe how our method is accounting for the observational selection effects inside our reconstruction algorithm. Also, I demonstrate that the renormalization of the prior distribution function is mandatory to account for higher order contributions in the structure formation model, and finally a redshift-dependent bias factor is theoretically motivated and implemented into our method. The various refinements yield unbiased results of the dark matter until scales of k≤0.2 h Mpc^−1in the power spectrum and isotropize the galaxy catalogue down to distances of r∼20h^−1 Mpc in the correlation function. We further test the results of our cosmic velocity field reconstruction by comparing them to a synthetic mock galaxy catalogue, finding a strong correlation between the mock and the reconstructed velocities. The applications of both, the density field without redshift-space distortions, and the velocity reconstructions, are very broad and can be used for improved analyses of the baryonic acoustic oscillations, environmental studies of the cosmic web, the kinematic Sunyaev-Zel’dovic or integrated Sachs-Wolfe effect. N2 - In der gegenwärtigen Anschauung der Kosmologie wird die Bildung von großräumigen Strukturen vor allem durch nicht strahlende, Dunkle Materie beeinflusst, die den überwiegenden Teil des Materieanteils des Universums ausmacht. Kosmologische Beobachtungen beruhen jedoch auf dem Nachweis von leuchtenden Galaxien, die gebiaste Indikatoren (biased tracer) der darunterliegenden Dunklen Materie sind. In dieser Arbeit präsentiere ich Rekonstruktionen des kosmischen Netzes der Dunklen Materie und kosmischer Geschwindigkeitsfelder. Beide Aspekte meiner Arbeit, der theoretische Formalismus und die Ergebnisse der Anwendungen sowohl auf kosmologische Simulationen als auch auf Galaxie-Rotverschiebungssurveys, weden detaiiert aufgeführt. Die Grundlage dieser Methode beruht auf einem statistischen Ansatz, bei dem ein gegebener Galaxienkatalog als eine Realisierung des darunter liegenden Dunklen Materiedichtefeldes interpretiert wird. Unsere Rekonstruktionen werden rechnerisch auf einem Gitter durch das Sampling einer Wahrscheinlichkeitsdichtefunktion durchgeführt, die die gemeinsame a posteriori Wahrscheinlichkeit der Materiedichte und des dreidimensionalen Geschwindigkeitsfeldes beschreibt. Der statistische Hintergrund unserer Methode ist im Kapitel "Implantation of argo" beschrieben, wobei die Einführung in die Samplingmethoden unter besonderer Berücksichtigung der Markov-Kette-Monte-Carlo-Technik erfolgt. Im Kapitel "Phase-Space Reconstructions with N-body Simulations" stelle ich ein neuartiges Biasmodell vor, welches die Galaxienanzahldichte mit der darunter liegenden Dunklen Materiedichte verknüpft. Diesen zerlege ich in einen deterministischen, nicht linearen und skalenabhängigen analytischen Teil und einen stochastischen Teil. Das letztere beschreibe ich durch einen Negativ-Binomial-Likelihood Ausdruck, welches die Abweichungen von Poissonität modelliert. Beide Biaskomponenten wurden bereits theoretisch untersucht, aber bisher noch nie in einem Rekonstruktionsalgorithmus getestet. Ich evaluiere diese neuen Beiträge mit $N$-Körper-Simulationen, um die Verbesserungen zu beurteilen und um zu zeigen, dass der stochastische Bias im Leistungsspektrum bei Wellenzahlen von k < 0.15 h Mpc^- 1 unabdingbar ist. Im zweiten Teil des Kapitels "Phase-Space Reconstructions with N-body Simulations" beschreibe und validiere ich unseren Ansatz, das kosmische Geschwindigkeitsfeld gemeinsam mit der Dunklen Materiedichte zu rekonstruieren. Ich verwende lineare Störungstheorie für die großräumigen Potentialströme und einen Dispersionsterm, um virialisierte Galaxiebewegungen zu modellieren. Die Ergebnisse zeigen, dass unsere Methode die Rotverschiebungsverzerrungen der Positionen der Galaxien genau beschreibt. Ich analysiere die Ergebnisse sowohl mit dem anisotropen Leistungsspektrum, als auch mit dem zweidimensionalen Leistungsspektrum. Schließlich zeige ich im Kapitel "Phase-space Reconstructions with Galaxy Redshift Surveys", wie ich alle Ergebnisse kombiniere und die Methode auf den CMASS (für Constant (stellar) Mass) Galaxienkatalog anwende. Ich beschreibe, wie unsere Methode die Selektionseffekte der Beobachtungen innerhalb des Rekonstruktionsalgorithmus berücksichtigt. Weiterhin demonstriere ich, dass die Renormalisierung der a priori Verteilung zwingend erforderlich ist, um die Beiträge höherer Ordnung im Strukturbildungsmodell zu berücksichtigen. Außerdem wird ein rotverschiebungsabhängiger Bias-Faktor theoretisch motiviert und in unseren Algorithmus implementiert. Unsere Rekonstruktionen, welche diese verschiedenen Verfeinerungen beinhaten, führen zu robusten Ergebnissen hinsichtlich des Feldes der Dunklen Materie bis zu Skalen von k <0.2 Mpc^-1 im Leistungsspektrum. Außerdem werden Anisotropien in dem rekonstruierten Galaxienkatalog bis zu Abständen von r~20 h^-1 Mpc in der Korrelationsfunktion zu einem hohen Grad überwunden. Wir testen die Ergebnisse unserer kosmischen Geschwindigkeitsrekonstruktion, indem wir sie mit einem synthetischen Mock-Galaxienkatalog vergleichen und bestätigen eine starke Korrelation zwischen den Mock- und den rekonstruierten Geschwindigkeiten. Die Anwendungen sowohl des Dichtefeldes ohne Rotverschiebungsverzerrungen als auch der Geschwindigkeitsrekonstruktionen sind sehr vielfältig und können für verbesserte Analysen der baryonischen akustischen Oszillationen, Umgebungsstudien des kosmischen Netzes, des kinematischen Sunjajew-Seldowitsch-Effekts oder des integrierten Sachs-Wolfe-Effekts verwendet werden. KW - large-scale structure formation KW - großräumige Strukturen KW - Kosmologie KW - Theorie KW - cosmology KW - theory Y1 - 2016 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-403565 ER - TY - THES A1 - Atmanspacher, Harald T1 - Informationsdynamik : Grundlagen, Interpretation, Konsequenzen Y1 - 1994 ER - TY - THES A1 - Auch, Mark T1 - Langsame Moleküldiffusion in Lipid-/Polyelektrolytmultischichten Y1 - 1999 ER - TY - JOUR A1 - Audenaert, Katrien A1 - Eisert, Jens A1 - Jane, E. A1 - Plenio, M. B. A1 - Virmani, S. A1 - Moor, B. D. T1 - The asymptotic relative entropy of entanglement N2 - We present an analytical formula for the asymptotic relative entropy of entanglement for Werner states of arbitrary dimensionality. We then demonstrate its validity using methods from convex optimization. This is the first case in which the value of a subadditive entanglement measure has been obtained in the asymptotic limit. This formula also gives the sharpest known upper bound on the distillable entanglement of these states. Y1 - 2001 ER - TY - THES A1 - Aue, Lars T1 - Cyclone impacts on sea ice in the Atlantic Arctic Ocean T1 - Auswirkungen von Zyklonen auf das Meereis im Atlantischen Arktischen Ozean N2 - The Arctic is the hot spot of the ongoing, global climate change. Over the last decades, near-surface temperatures in the Arctic have been rising almost four times faster than on global average. This amplified warming of the Arctic and the associated rapid changes of its environment are largely influenced by interactions between individual components of the Arctic climate system. On daily to weekly time scales, storms can have major impacts on the Arctic sea-ice cover and are thus an important part of these interactions within the Arctic climate. The sea-ice impacts of storms are related to high wind speeds, which enhance the drift and deformation of sea ice, as well as to changes in the surface energy budget in association with air mass advection, which impact the seasonal sea-ice growth and melt. The occurrence of storms in the Arctic is typically associated with the passage of transient cyclones. Even though the above described mechanisms how storms/cyclones impact the Arctic sea ice are in principal known, there is a lack of statistical quantification of these effects. In accordance with that, the overarching objective of this thesis is to statistically quantify cyclone impacts on sea-ice concentration (SIC) in the Atlantic Arctic Ocean over the last four decades. In order to further advance the understanding of the related mechanisms, an additional objective is to separate dynamic and thermodynamic cyclone impacts on sea ice and assess their relative importance. Finally, this thesis aims to quantify recent changes in cyclone impacts on SIC. These research objectives are tackled utilizing various data sets, including atmospheric and oceanic reanalysis data as well as a coupled model simulation and a cyclone tracking algorithm. Results from this thesis demonstrate that cyclones are significantly impacting SIC in the Atlantic Arctic Ocean from autumn to spring, while there are mostly no significant impacts in summer. The strength and the sign (SIC decreasing or SIC increasing) of the cyclone impacts strongly depends on the considered daily time scale and the region of the Atlantic Arctic Ocean. Specifically, an initial decrease in SIC (day -3 to day 0 relative to the cyclone) is found in the Greenland, Barents and Kara Seas, while SIC increases following cyclones (day 0 to day 5 relative to the cyclone) are mostly limited to the Barents and Kara Seas. For the cold season, this results in a pronounced regional difference between overall (day -3 to day 5 relative to the cyclone) SIC-decreasing cyclone impacts in the Greenland Sea and overall SIC-increasing cyclone impacts in the Barents and Kara Seas. A cyclone case study based on a coupled model simulation indicates that both dynamic and thermodynamic mechanisms contribute to cyclone impacts on sea ice in winter. A typical pattern consisting of an initial dominance of dynamic sea-ice changes followed by enhanced thermodynamic ice growth after the cyclone passage was found. This enhanced ice growth after the cyclone passage most likely also explains the (statistical) overall SIC-increasing effects of cyclones in the Barents and Kara Seas in the cold season. Significant changes in cyclone impacts on SIC over the last four decades have emerged throughout the year. These recent changes are strongly varying from region to region and month to month. The strongest trends in cyclone impacts on SIC are found in autumn in the Barents and Kara Seas. Here, the magnitude of destructive cyclone impacts on SIC has approximately doubled over the last four decades. The SIC-increasing effects following the cyclone passage have particularly weakened in the Barents Sea in autumn. As a consequence, previously existing overall SIC-increasing cyclone impacts in this region in autumn have recently disappeared. Generally, results from this thesis show that changes in the state of the sea-ice cover (decrease in mean sea-ice concentration and thickness) and near-surface air temperature are most important for changed cyclone impacts on SIC, while changes in cyclone properties (i.e. intensity) do not play a significant role. N2 - Die Arktis ist der Hotspot des globalen Klimawandels. In den letzten Jahrzehnten sind die oberflächennahen Temperaturen in der Arktis fast viermal so schnell gestiegen wie im globalen Durchschnitt. Diese verstärkte Erwärmung der Arktis und die damit verbundenen raschen Umweltveränderungen werden u.a. durch Wechselwirkungen zwischen den einzelnen Komponenten des arktischen Klimasystems angetrieben. Auf täglichen bis wöchentlichen Zeitskalen können Stürme große Einflüsse auf das arktische Meereis haben und sind somit ein wichtiger Teil dieser Wechselwirkungen innerhalb des arktischen Klimas. Der Einfluss der Stürme auf das Meereis resultiert aus den hohen Windgeschwindigkeiten, welche die Drift und Verformung des Meereises verstärken, sowie aus Änderungen in der Oberflächenenergiebilanz im Zusammenhang mit der Advektion von Luftmassen, was das Wachstum und Schmelzen des Meereises beeinflusst. Das Auftreten von Stürmen in der Arktis ist oft mit dem Durchzug von Zyklonen verbunden. Obwohl die oben beschriebenen Mechanismen, wie sich Stürme/Zyklone auf das arktische Meereis auswirken, im Prinzip bekannt sind, fehlt es an einer statistischen Quantifizierung dieser Effekte. Dementsprechend ist das übergeordnete Ziel dieser Arbeit eine statistische Quantifizierung der Auswirkungen von Zyklonen auf die Meereiskonzentration (engl. Sea Ice Concentration, SIC) im atlantischen Arktischen Ozeans über die letzten vier Jahrzehnte. Um ein Verständnis für die zugrunde liegenden Mechanismen zu erlangen, besteht ein weiteres Ziel darin, die dynamischen und thermodynamischen Auswirkungen von Zyklonen auf das Meereis zu trennen und ihre relative Bedeutung zu analysieren. Zuletzt zielt diese Arbeit darauf ab, aktuelle Veränderungen der Zykloneneinflüsse auf das Meereis zu quantifizieren. Zum Erreichen dieser Forschungsziele werden verschiedene Datensätze genutzt, darunter atmosphärische und ozeanische Reanalysedaten sowie eine gekoppelte Modellsimulation und ein Algorithmus zur automatischen Identifikation von Zyklonen. Die Ergebnisse dieser Arbeit zeigen, dass Zyklone die SIC im atlantischen Arktischen Ozean von Herbst bis Frühjahr signifikant beeinflussen, während es im Sommer meist keine signifikanten Auswirkungen gibt. Die Stärke und das Vorzeichen (abnehmende oder zunehmende SIC) der Auswirkungen der Zyklone hängt stark von der betrachteten täglichen Zeitskala und der Region des Arktischen Ozeans ab. So ist ein anfänglicher Rückgang der SIC (Tag -3 bis Tag 0 relativ zum Zyklonendurchgang) in der Grönland-, der Barents- und der Karasee festzustellen, während ein SIC-Anstieg nach dem Zyklonendurchgang (Tag 0 bis Tag 5 relativ zum Zyklonendurchgang) hauptsächlich auf die Barents- und die Karasee beschränkt ist. Für die kalte Jahreszeit ergibt sich daraus ein ausgeprägter regionaler Unterschied zwischen insgesamt (Tag -3 bis Tag 5 relativ zum Zyklon) SIC-verringernden Zyklonenauswirkungen in der Grönlandsee und insgesamt SIC-erhöhenden Zyklonenauswirkungen in der Barents- und Karasee. Die Analyse spezifischer Zyklonenfälle basierend auf einer gekoppelten Modellsimulation zeigt, dass sowohl dynamische als auch thermodynamische Mechanismen zu den Auswirkungen von Zyklonen auf das Meereis im Winter beitragen. Hierbei wurde ein typisches Muster bestehend aus einer anfänglichen Dominanz dynamischer Meereisveränderungen gefolgt von verstärktem thermodynamischem Eiswachstum nach der Zyklonenpassage gefunden. Dieses verstärkte Eiswachstum nach der Zyklonenpassage erklärt u.a. auch die (statistischen) insgesamt SIC-erhöhenden Effekte von Zyklonen in der Barents- und Karasee im Winter. Signifikante Änderungen in den Auswirkungen von Zyklonen auf die SIC über die letzten vier Dekaden sind das ganze Jahr über zu finden. Diese Veränderungen variieren stark von Region zu Region und von Monat zu Monat. Die stärksten Trends in den Auswirkungen von Zyklonen auf die SIC sind im Herbst in der Barents- und Karasee zu beobachten. Hier hat sich die Stärke der zerstörerischen Auswirkungen von Zyklonen auf die SIC in den letzten vier Jahrzehnten ungefähr verdoppelt. Die SIC-erhöhenden Effekte nach der Zyklonenpassage haben sich in der Barentssee im Herbst besonders abgeschwächt. Dadurch sind zuvor existierende, insgesamt SIC-erhöhende Zyklonenauswirkungen in dieser Region und Jahreszeit zuletzt verschwunden. Generell zeigen die Ergebnisse dieser Arbeit, dass Änderungen im Zustand des Meereises (Abnahme der mittleren Meereiskonzentration und -dicke) sowie in der Lufttemperatur die veränderten Auswirkungen der Zyklonen auf die SIC antreiben, während Veränderungen in den Eigenschaften der Zyklonen (z.B. ihre Intensität) keine wesentliche Rolle spielen. KW - Arctic KW - atmosphere KW - sea ice KW - cyclones KW - meteorology KW - Arktis KW - Atmosphäre KW - Meereis KW - Zyklone KW - Meteorologie Y1 - 2024 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-634458 SP - VIII, 131 ER - TY - THES A1 - Aulbert, Carsten T1 - Finding millisecond binary pulsars in 47 tucanae by applying the hough transformation to radio data Y1 - 2005 CY - Potsdam ER - TY - THES A1 - Auraß, Henry T1 - Radiobeobachtungen der Sonnenkorona - ein Zugang zur Flarephysik : einige experimentelle Beiträge zum Verständnis der Dynamik des Flarerozesses Y1 - 1994 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 - JOUR A1 - Avilov, Anatoly S. A1 - Kulygin, Alexander K. A1 - Pietsch, Ullrich A1 - Spence, John C. H. A1 - Tsirelson, Vladimir G. A1 - Zuo, Ming J. T1 - Scanning system for high-energy electron diffractometry Y1 - 1999 UR - http://www3.interscience.wiley.com/journal/118518709/home?CRETRY=1&SRETRY=0 U6 - https://doi.org/10.1107/S0021889899006755 SN - 0021-8898 ER - TY - JOUR A1 - Avilov, Anatoly S. A1 - Lepeshov, G. G. A1 - Pietsch, Ullrich A1 - Tsirelson, Vladimir G. T1 - Multipole analysis of the electron density and electrostatic potential in Germanium by high-resolution electron diffraction Y1 - 2001 SN - 0022-3697 ER - TY - JOUR A1 - Awad, Emad A1 - Metzler, Ralf T1 - Crossover dynamics from superdiffusion to subdiffusion BT - models and solutions JF - Fractional calculus and applied analysis : an international journal for theory and applications N2 - The Cattaneo or telegrapher's equation describes the crossover from initial ballistic to normal diffusion. Here we study and survey time-fractional generalisations of this equation that are shown to produce the crossover of the mean squared displacement from superdiffusion to subdiffusion. Conditional solutions are derived in terms of Fox H-functions and the dth-order moments as well as the diffusive flux of the different models are derived. Moreover, the concept of the distribution-like is proposed as an alternative to the probability density function. KW - Cattaneo equation KW - telegrapher's equation KW - crossover dynamics KW - fractional dynamic equations KW - anomalous diffusion KW - superdiffusion and KW - subdiffusion KW - Fox H-functions Y1 - 2020 U6 - https://doi.org/10.1515/fca-2020-0003 SN - 1311-0454 SN - 1314-2224 VL - 23 IS - 1 SP - 55 EP - 102 PB - De Gruyter CY - Berlin ; Boston ER - TY - JOUR A1 - Awad, Emad A1 - Metzler, Ralf T1 - Closed-form multi-dimensional solutions and asymptotic behaviours for subdiffusive processes with crossovers: II. Accelerating case JF - Journal of physics : A, Mathematical and theoretical N2 - Anomalous diffusion with a power-law time dependence vertical bar R vertical bar(2)(t) similar or equal to t(alpha i) of the mean squared displacement occurs quite ubiquitously in numerous complex systems. Often, this anomalous diffusion is characterised by crossovers between regimes with different anomalous diffusion exponents alpha(i). Here we consider the case when such a crossover occurs from a first regime with alpha(1) to a second regime with alpha(2) such that alpha(2) > alpha(1), i.e., accelerating anomalous diffusion. A widely used framework to describe such crossovers in a one-dimensional setting is the bi-fractional diffusion equation of the so-called modified type, involving two time-fractional derivatives defined in the Riemann-Liouville sense. We here generalise this bi-fractional diffusion equation to higher dimensions and derive its multidimensional propagator (Green's function) for the general case when also a space fractional derivative is present, taking into consideration long-ranged jumps (Levy flights). We derive the asymptotic behaviours for this propagator in both the short- and long-time as well the short- and long-distance regimes. Finally, we also calculate the mean squared displacement, skewness and kurtosis in all dimensions, demonstrating that in the general case the non-Gaussian shape of the probability density function changes. KW - multidimensional fractional diffusion equation KW - continuous time random KW - walks KW - crossover anomalous diffusion dynamics KW - non-Gaussian probability KW - density Y1 - 2022 U6 - https://doi.org/10.1088/1751-8121/ac5a90 SN - 1751-8113 SN - 1751-8121 VL - 55 IS - 20 PB - IOP Publ. Ltd. CY - Bristol 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 - Aydiner, Ekrem A1 - Cherstvy, Andrey G. A1 - Metzler, Ralf T1 - Money distribution in agent-based models with position-exchange dynamics BT - the Pareto paradigm revisited JF - The European physical journal : B, Condensed matter and complex systems N2 - Wealth and income distributions are known to feature country-specific Pareto exponents for their long power-law tails. To propose a rationale for this, we introduce an agent-based dynamic model and use Monte Carlo simulations to unveil the wealth distributions in closed and open economical systems. The standard money-exchange scenario is supplemented with the position-exchange agent dynamics that vitally affects the Pareto law. Specifically, in closed systems with position-exchange dynamics the power law changes to an exponential shape, while for open systems with traps the Pareto law remains valid. KW - Statistical and Nonlinear Physics Y1 - 2019 U6 - https://doi.org/10.1140/epjb/e2019-90674-0 SN - 1434-6028 SN - 1434-6036 VL - 92 IS - 5 PB - Springer CY - New York 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 - BOOK A1 - Backhaus, Udo ED - Mikelskis, Helmut ED - Wilke, Hans-Joachim ED - Schön, Lutz-Helmut T1 - Physik plus : Kl. 9/10, [Hauptbd.], Gymnasium Nordrhein-Westfalen Y1 - 2002 SN - 3-06-020980-4 PB - Volk und Wissen CY - Berlin ER - TY - BOOK A1 - Backhaus, Udo A1 - Schön, Lutz-Helmut ED - Mikelskis, Helmut ED - Wilke, Hans-Joachim T1 - Physik plus : Kl. 8, [Hauptbd.], Gymnasium Nordrhein-Westfalen Y1 - 2001 SN - 3-06-020840-9 PB - Volk und Wissen Verl. CY - Berlin ER - TY - THES A1 - Baczyński, Krzysztof Konrad T1 - Buckling instabilities of semiflexible filaments in biological systems T1 - Knickinstabilitäten semiflexibler Filamente in biologischen Systemen N2 - In dieser Arbeit werden Knickinstabilitäten von Filamenten in biologischen Systemen untersucht. Das Zytoskelett von Zellen ist aus solchen Filamenten aufgebaut. Sie sind für die mechanische Stabilität der Zelle verantwortlich und spielen eine große Rolle bei intrazellulären Transportprozessen durch molekulare Motoren, die verschiedene Lasten wie beispielsweise Organellen entlang der Filamente des Zytoskeletts transportieren. Filamente sind semiflexible Polymere, deren Biegeenergie ähnlich groß ist wie die thermische Energie, so dass sie auch als elastische Balken auf der Nanoskala gesehen werden können, die signifikante thermische Fluktuationen zeigen. Wie ein makroskopischer elastischer Balken können auch Filamente eine mechanische Knickinstabilität unter Kompression zeigen. Im ersten Teil dieser Arbeit wird untersucht, wie diese Instabilität durch thermische Fluktuationen der Filamente beeinflusst wird. In Zellen können Kompressionskräfte durch molekulare Motoren erzeugt werden. Das geschieht zum Beispiel während der Zellteilung in der mitotischen Spindel. Im zweiten Teil der Arbeit untersuchen wir, wie die stochastische Natur einer von Motoren generierten Kraft die Knickinstabilität von Filamenten beeinflusst. Zunächst stellen wir kurz das Problem von Knickinstabilitäten auf der makroskopischen Skala dar und führen ein Modell für das Knicken von Filamenten oder elastischen Stäben in zwei Raumdimensionen und in Anwesenheit thermischer Fluktuationen ein. Wir präsentieren eine analytische Lösung für Knickinstabilitäten in Anwesenheit thermischer Fluktuationen, die auf einer Renormierungsgruppenrechnung im Rahmen des nichtlinearen Sigma-Models basiert. Wir integrieren die kurzwelligen Fluktuationen aus, um eine effektive Theorie für die langwelligen Moden zu erhalten, die die Knickinstabilität bestimmen. Wir berechnen die Änderung der kritischen Kraft für die Knickinstabilität und zeigen, dass die thermischen Fluktuationen in zwei Raumdimensionen zu einer Zunahme der kritischen Kraft führen. Außerdem zeigen wir, dass thermische Fluktuationen im geknickten Zustand zu einer Zunahme der mittleren projizierten Länge des Filaments in Richtung der wirkenden Kraft führen. Als Funktion der Konturlänge des Filaments besitzt die mittlere projizierte Länge eine Spitze an der Knickinstabilität, die durch thermische Fluktuationen abgerundet wird. Unser Hauptresultat ist die Beobachtung, dass ein geknicktes Filament unter dem Einfluss thermischer Fluktuationen gestreckt wird, d.h. dass seine mittlere projizierte Länge in Richtung der Kompressionskraft auf Grund der thermischen Fluktuationen zunimmt. Unsere analytischen Resultate werden durch Monte-Carlo Simulationen der Knickinstabilität semiflexibler Filamente in zwei Raumdimensionen bestätigt. Wir führen auch Monte-Carlo Simulationen in höheren Raumdimensionen durch und zeigen, dass die Zunahme der projizierten Länge unter dem Einfluss thermischer Fluktuationen weniger ausgeprägt ist und stark von der Wahl der Randbedingungen abhängt. Im zweiten Teil der Arbeit formulieren wir ein Modell für die Knickinstabilität semiflexibler Filamente unter dem Einfluss molekularer Motoren. Wir untersuchen ein System, in dem sich eine Gruppe von Motoren entlang eines fixierten Filaments bewegt, und dabei ein zweites Filament als Last trägt. Das Last-Filament wird gegen eine Wand gedrückt und knickt. Während des Knickvorgangs können die Motoren, die die Kraft auf das Filament generieren, stochastisch von dem Filament ab- und an das Filament anbinden. Wir formulieren ein stochastisches Model für dieses System und berechnen die “mean first passage time“, d.h. die mittlere Zeit für den Übergang von einem Zustand, in dem alle Motoren gebundenen sind zu einem Zustand, in dem alle Motoren abgebunden sind. Dieser Übergang entspricht auch einem Übergang aus dem gebogenen zurück in einen ungebogenen Zustand des Last-Filaments. Unser Resultat zeigt, dass für genügend kurze Mikrotubuli die Bewegung der Motoren von der durch das Last-Filament generierten Kraft beeinflusst wird. Diese Ergebnisse können in zukünftigen Experimenten überprüft werden. N2 - We study buckling instabilities of filaments in biological systems. Filaments in a cell are the building blocks of the cytoskeleton. They are responsible for the mechanical stability of cells and play an important role in intracellular transport by molecular motors, which transport cargo such as organelles along cytoskeletal filaments. Filaments of the cytoskeleton are semiflexible polymers, i.e., their bending energy is comparable to the thermal energy such that they can be viewed as elastic rods on the nanometer scale, which exhibit pronounced thermal fluctuations. Like macroscopic elastic rods, filaments can undergo a mechanical buckling instability under a compressive load. In the first part of the thesis, we study how this buckling instability is affected by the pronounced thermal fluctuations of the filaments. In cells, compressive loads on filaments can be generated by molecular motors. This happens, for example, during cell division in the mitotic spindle. In the second part of the thesis, we investigate how the stochastic nature of such motor-generated forces influences the buckling behavior of filaments. In chapter 2 we review briefly the buckling instability problem of rods on the macroscopic scale and introduce an analytical model for buckling of filaments or elastic rods in two spatial dimensions in the presence of thermal fluctuations. We present an analytical treatment of the buckling instability in the presence of thermal fluctuations based on a renormalization-like procedure in terms of the non-linear sigma model where we integrate out short-wavelength fluctuations in order to obtain an effective theory for the mode of the longest wavelength governing the buckling instability. We calculate the resulting shift of the critical force by fluctuation effects and find that, in two spatial dimensions, thermal fluctuations increase this force. Furthermore, in the buckled state, thermal fluctuations lead to an increase in the mean projected length of the filament in the force direction. As a function of the contour length, the mean projected length exhibits a cusp at the buckling instability, which becomes rounded by thermal fluctuations. Our main result is the observation that a buckled filament is stretched by thermal fluctuations, i.e., its mean projected length in the direction of the applied force increases by thermal fluctuations. Our analytical results are confirmed by Monte Carlo simulations for buckling of semiflexible filaments in two spatial dimensions. We also perform Monte Carlo simulations in higher spatial dimensions and show that the increase in projected length by thermal fluctuations is less pronounced than in two dimensions and strongly depends on the choice of the boundary conditions. In the second part of this work, we present a model for buckling of semiflexible filaments under the action of molecular motors. We investigate a system in which a group of motors moves along a clamped filament carrying a second filament as a cargo. The cargo-filament is pushed against the wall and eventually buckles. The force-generating motors can stochastically unbind and rebind to the filament during the buckling process. We formulate a stochastic model of this system and calculate the mean first passage time for the unbinding of all linking motors which corresponds to the transition back to the unbuckled state of the cargo filament in a mean-field model. Our results show that for sufficiently short microtubules the movement of kinesin-I-motors is affected by the load force generated by the cargo filament. Our predictions could be tested in future experiments. KW - Polymere KW - Filament KW - Elastizität KW - Knickinstabilität KW - molekulare Motoren KW - Polymers KW - filaments KW - elasticity KW - buckling KW - molecular motors Y1 - 2009 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-37927 ER - TY - JOUR A1 - Bae, Albert J. A1 - Beta, Carsten A1 - Bodenschatz, Eberhard T1 - Rapid switching of chemical signals in microfluidic devices N2 - We present an analysis of concentration switching times in microfluidic devices. The limits of rapid switching are analyzed based on the theory of dispersion by Taylor and Aris and compared to both experiments and numerical simulations. We focus on switching times obtained by photo-activation of caged compounds in a micro-flow (flow photolysis). The performance of flow photolysis is compared to other switching techniques. A flow chart is provided to facilitate the application of our theoretical analysis to microfluidic switching devices. Y1 - 2009 UR - http://pubs.rsc.org/en/Journals/JournalIssues/LC U6 - https://doi.org/10.1039/B905521e SN - 1473-0197 ER - TY - THES A1 - Bae, Sung-Min T1 - Nichtlinear optische Untersuchungen an Adsorptionsschichten löslicher Amphiphile - Überprüfung thermodynamischer Modelle Y1 - 1999 ER - TY - JOUR A1 - Bagnich, Sergey A. A1 - Bassler, H. A1 - Neher, Dieter T1 - Sensitized phosphorescence of benzil-doped ladder-type methyl-poly(para-phenylene) N2 - The delayed luminescence and phosphorescence of ladder-type methyl-poly(para-phenylene) (MeLPPP) doped with benzil at a concentration of 20% by weight has been measured. The introduction of benzil leads to a dramatic reduction of the polymer singlet emission. At the same time, a new band with maximum at 611 nm appears, corresponding to the phosphorescence of MeLPPP. The phosphorescence decay on the short time scale is close to an exponential law with a time decay of 15 ms. This indicates that benzil can efficiently sensitize the phosphorescence of the polymer. In addition, a broad and featureless emission is observed in the delayed luminescence spectra of benzil-doped MeLPPP, which is attributed to an exciplex formed between the polymer host and the dopant. We further observe that the delayed fluorescence is enhanced by the addition of benzil. It is concluded that the delayed fluorescence of benzil-doped MeLPPP is mainly due to the annihilation of triplet excitons on the polymer. Finally, efficient triplet-triplet energy transfer from the benzil-doped polymer to the red-emitting phosphorescent dye Pt(II)octaethylporphyrin is established. (C) 2004 American Institute of Physics Y1 - 2004 SN - 0021-9606 ER - TY - JOUR A1 - Bagnich, Sergey A. A1 - Bassler, H. A1 - Neher, Dieter T1 - Exciton dynamics in ladder-type methyl-poly(para-phenylene) doped with phosphorescent dyes N2 - The luminescence of a ladder-type methyl-poly(para-phenylene) (MeLPPP) doped with platinum-porphyrin dye PtOEP covering the concentration 10(-3)-5% by weight has been measured employing cw and transient techniques. Upon excitation into the range of absorption of the host, strong phosphorescence of the dopant is observed. Possible ways of populating the dopant triplet state are considered. (c) 2004 Elsevier B.V. All rights reserved Y1 - 2005 SN - 0022-2313 ER - TY - JOUR A1 - Bagnich, Sergey A. A1 - Im, C. A1 - Bassler, H. A1 - Neher, Dieter A1 - Scherf, Ullrich T1 - Energy transfer in a ladder-type methyl-poly(para-phenylene) doped by Pt(II)octaethylporphyrin N2 - The luminescence of a ladder-type methyl-poly(para-phenylene) (MeLPPP) doped by platinum-porphyrin dye PtOEP covering the concentration 10(-3) to 5% by weight has been measured employing cw and transient techniques. Upon excitating into the range of absorption of the host strong phosphorescence of the dopant is observed. Possible ways of populating of the dopant triplet state are considered. It is shown that the main channel is singlet-singlet energy transfer among chromophor groups of the polymer followed by Forster-type transfer to the guest and subsequent intersystem crossing. (C) 2003 Elsevier B.V. All rights reserved Y1 - 2004 SN - 0301-0104 ER - TY - JOUR A1 - Bagnich, Sergey A. A1 - Unger, Th. A1 - Jaiser, Frank A1 - Neher, Dieter A1 - Thesen, M. W. A1 - Krüger, H. T1 - Efficient green electrophosphorescence based on ambipolar nonconjugated polymers evaluation of transport and emission properties JF - Journal of applied physics N2 - New materials for polymer organic light-emitting diodes based on a polymer matrix doped with phosphorescent dyes are presented. The matrix system is based on a polystyrene backbone bearing either electron or hole transporting units at the 4-position of each repeat unit. Random copolymers and polymer blend systems of the homopolymers are prepared, both with 62 wt.% electron transporting and 38 wt.% hole transporting moieties. Adding a green electrophosphorescent dye to the polymer matrix leads to efficient electroluminescence with a maximum current efficiency of 35 cd/A and a maximum external quantum efficiency of up to 10%. The mobilities of electrons and holes in the dye-doped copolymer, as measured by transient electroluminescence, are around 5 x 10(-5) and 5 x 10(-6) cm(2)/Vs, respectively, while the blend of the two homopolymers exhibits slightly lower mobilities of both types of carriers. Despite the pronounced imbalance of charge transport, the device performance is almost entirely limited by the phosphorescence efficiency of the dye, implying balanced flow of holes and electrons into the active region. Also, devices made with either the copolymer or the blend yielded very similar device efficiencies, despite the noticeable difference in electron and hole mobility. It is proposed that electrons are efficiently blocked at the interlayer and that the so-formed space charge assists the balanced injection of holes. Y1 - 2011 U6 - https://doi.org/10.1063/1.3618681 SN - 0021-8979 SN - 1089-7550 VL - 110 IS - 3 PB - American Institute of Physics CY - Melville ER - TY - THES A1 - Bahr, Benjamin T1 - Analysis of the Loop Quantum Gravity dynamics with coherent states and categories Y1 - 2008 CY - Potsdam ER - TY - JOUR A1 - Baibolatov, Yernur A1 - Rosenblum, Michael A1 - Zhanabaev, Zeinulla Zh. A1 - Kyzgarina, Meyramgul A1 - Pikovskij, Arkadij T1 - Periodically forced ensemble of nonlinearly coupled oscillators : from partial to full synchrony N2 - We analyze the dynamics of a periodically forced oscillator ensemble with global nonlinear coupling. Without forcing, the system exhibits complicated collective dynamics, even for the simplest case of identical phase oscillators: due to nonlinearity, the synchronous state becomes unstable for certain values of the coupling parameter, and the system settles at the border between synchrony and asynchrony, what can be denoted as partial synchrony. We find that an external common forcing can result in two synchronous states: (i) a weak forcing entrains only the mean field, whereas the individual oscillators remain unlocked to the force and, correspondingly, to the mean field; (ii) a strong forcing fully synchronizes the system, making the phases of all oscillators identical. Analytical results are confirmed by numerics. Y1 - 2009 UR - http://pre.aps.org/ U6 - https://doi.org/10.1103/PhysRevE.80.046211 SN - 1539-3755 ER - TY - JOUR A1 - Baibolatov, Yernur A1 - Rosenblum, Michael A1 - Zhanabaev, Zeinulla Zh. A1 - Pikovskij, Arkadij T1 - Complex dynamics of an oscillator ensemble with uniformly distributed natural frequencies and global nonlinear coupling N2 - We consider large populations of phase oscillators with global nonlinear coupling. For identical oscillators such populations are known to demonstrate a transition from completely synchronized state to the state of self-organized quasiperiodicity. In this state phases of all units differ, yet the population is not completely incoherent but produces a nonzero mean field; the frequency of the latter differs from the frequency of individual units. Here we analyze the dynamics of such populations in case of uniformly distributed natural frequencies. We demonstrate numerically and describe theoretically (i) states of complete synchrony, (ii) regimes with coexistence of a synchronous cluster and a drifting subpopulation, and (iii) self-organized quasiperiodic states with nonzero mean field and all oscillators drifting with respect to it. We analyze transitions between different states with the increase of the coupling strength; in particular we show that the mean field arises via a discontinuous transition. For a further illustration we compare the results for the nonlinear model with those for the Kuramoto-Sakaguchi model. Y1 - 2010 UR - http://pre.aps.org/ U6 - https://doi.org/10.1103/Physreve.82.016212 SN - 1539-3755 ER - TY - JOUR A1 - Baibolatov, Yernur A1 - Spahn, Frank T1 - The role of adhesion for ensembles of mesoscopic particles JF - Granular matter N2 - We present a toy-model for an ensemble of adhering mesoscopic constituents in order to estimate the effect of the granular temperature on the sizes of embedded aggregates. The major goal is to illustrate the relation between the mean aggregate size and the granular temperature in dense planetary rings. For sake of simplicity we describe the collective behavior of the ensemble by means of equilibrium statistical mechanics, motivated by the stationary temperature established by the balance between a Kepler-shear driven viscous heating and inelastic cooling in these cosmic granular disks. The ensemble consists of N' equal constituents which can form cluster(s) or move like a gas-or both phases may coexist-depending on the (granular) temperature of the system. We assume the binding energy levels of a cluster E-c = -N-c gamma a to be determined by a certain contact number N-c, given by the configuration of N constituents of the aggregate (energy per contact: -gamma a). By applying canonical and grand-canonical ensembles, we show that the granular temperature T of a gas of constituents (their mean kinetic energy) controls the size distribution of the aggregates. They are the smaller the higher the granular temperature T is. A mere gas of single constituents is sustained for T >> gamma a. In the case of large clusters (low temperatures T << gamma a) the size distribution becomes a Poissonian. KW - Adhesion KW - Statistical mechanics KW - Planetary rings Y1 - 2012 U6 - https://doi.org/10.1007/s10035-012-0325-4 SN - 1434-5021 VL - 14 IS - 2 SP - 197 EP - 202 PB - Springer CY - New York ER - TY - JOUR A1 - Baier, Frank W. T1 - Dominant galaxies in bimodal cluster Y1 - 1994 ER - TY - THES A1 - Baier, Frank W. T1 - Strukturen von Galaxienhaufen und ihre Bedeutung für die Entwicklung der Haufen und ihrer zentralen dominierenden Galaxien Y1 - 2000 CY - Potsdam ER - TY - JOUR A1 - Baier, Frank W. A1 - Lima-Neto, G. B. A1 - Wipper, H. T1 - Comparison between optical and X-ray structures of galaxy clusters Y1 - 1996 ER - TY - JOUR A1 - Baier, Frank W. A1 - Lima-Neto, G. B. A1 - Wipper, H. A1 - Braun, Michael T1 - Optical and X-ray structures of galaxy clusters I Y1 - 1996 ER - TY - JOUR A1 - Baier, Frank W. A1 - McGillivray, H. T. A1 - Flin, P. A1 - Krywult, J. T1 - The imadmissibility of radial number density profiles of galaxy clusters Y1 - 1994 ER - TY - JOUR A1 - Baier, Frank W. A1 - Wipper, H. T1 - Compilation of nearby northern Abell clusters with central dominant galaxies Y1 - 1995 ER - TY - JOUR A1 - Baier, Frank W. A1 - Wipper, H. T1 - Luminosity distribution in cD clusters Y1 - 1994 ER -