TY - GEN A1 - Goychuk, Igor A. A1 - Kharchenko, Vasyl O. A1 - Metzler, Ralf T1 - Molecular motors pulling cargos in the viscoelastic cytosol: how power strokes beat subdiffusion T2 - Physical Chemistry Chemical Physics N2 - The discovery of anomalous diffusion of larger biopolymers and submicron tracers such as endogenous granules, organelles, or virus capsids in living cells, attributed to the viscoelastic nature of the cytoplasm, provokes the question whether this complex environment equally impacts the active intracellular transport of submicron cargos by molecular motors such as kinesins: does the passive anomalous diffusion of free cargo always imply its anomalously slow active transport by motors, the mean transport distance along microtubule growing sublinearly rather than linearly in time? Here we analyze this question within the widely used two-state Brownian ratchet model of kinesin motors based on the continuous-state diffusion along microtubules driven by a flashing binding potential, where the cargo particle is elastically attached to the motor. Depending on the cargo size, the loading force, the amplitude of the binding potential, the turnover frequency of the molecular motor enzyme, and the linker stiffness we demonstrate that the motor transport may turn out either normal or anomalous, as indeed measured experimentally. We show how a highly efficient normal active transport mediated by motors may emerge despite the passive anomalous diffusion of the cargo, and study the intricate effects of the elastic linker. Under different, well specified conditions the microtubule-based motor transport becomes anomalously slow and thus significantly less efficient. T3 - Zweitveröffentlichungen der Universität Potsdam : Mathematisch-Naturwissenschaftliche Reihe - 181 KW - royal soc chemistry KW - thomas graham house KW - science park KW - milton rd KW - cambridge cb4 0wf KW - cambs KW - england Y1 - 2014 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-76478 SP - 16524 EP - 16535 PB - The Royal Society of Chemistry CY - Cambridge ER - TY - JOUR A1 - Kusterer, D. -J. A1 - Nagel, T. A1 - Hartmann, S. A1 - Werner, K. A1 - Feldmeier, Achim T1 - Monte Carlo radiation transfer in CV disk winds: application to the AM CVn prototype JF - Astronomy and astrophysics : an international weekly journal N2 - Context. AMCVn systems are ultracompact binaries in which a (semi-) degenerate star transfers helium-dominated matter onto a white dwarf. They are effective gravitational-wave emitters and potential progenitors of Type Ia supernovae. Aims. To understand the evolution of AMCVn systems it is necessary to determine their mass-loss rate through their radiation-driven accretion-disk wind. We constructed models to perform quantitative spectroscopy of P Cygni line profiles that were detected in UV spectra. Methods. We performed 2.5D Monte Carlo radiative transfer calculations in hydrodynamic wind structures by making use of realistic NLTE spectra from the accretion disk and by accounting for the white dwarf as an additional photon source. Results. We present first results from calculations in which LTE opacities are used in the wind model. A comparison with UV spectroscopy of the AMCVn prototype shows that the modeling procedure is potentially a good tool for determining mass-loss rates and abundances of trace metals in the helium-rich wind. KW - radiative transfer KW - stars: winds, outflows KW - stars: individual: AM CVn KW - accretion, accretion disks Y1 - 2014 U6 - https://doi.org/10.1051/0004-6361/201321438 SN - 0004-6361 SN - 1432-0746 VL - 561 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Zink, Christof A1 - Werner, Nils A1 - Jechow, Andreas A1 - Heuer, Axel A1 - Menzel, Ralf T1 - Multi-wavelength operation of a single broad area diode laser by spectral beam combining JF - IEEE photonics technology letters N2 - Stabilized multi-wavelength emission from a single emitter broad area diode laser (BAL) is realized by utilizing an external cavity with a spectral beam combining architecture. Self-organized emitters that are equidistantly spaced across the slow axis are enforced by the spatially distributed wavelength selectivity of the external cavity. This resulted in an array like near-field emission although the BAL is physically a single emitter without any epitaxial sub-structuring and only one electrical contact. Each of the self-organized emitters is operated at a different wavelength and the emission is multiplexed into one spatial mode with near-diffraction limited beam quality. With this setup, multi-line emission of 31 individual spectral lines centered around and a total spectral width of 3.6 nm is realized with a 1000 mu m wide BAL just above threshold. To the best of our knowledge, this is the first demonstration of such a self-organization of emitters by optical feedback utilizing a spectral beam combining architecture. KW - Laser resonators KW - semiconductor lasers KW - optical feedback Y1 - 2014 U6 - https://doi.org/10.1109/LPT.2013.2291963 SN - 1041-1135 SN - 1941-0174 VL - 26 IS - 3 SP - 253 EP - 256 PB - Inst. of Electr. and Electronics Engineers CY - Piscataway ER - TY - THES A1 - Fischer, Jost Leonhardt T1 - Nichtlineare Kopplungsmechanismen akustischer Oszillatoren am Beispiel der Synchronisation von Orgelpfeifen T1 - Nonlinear coupling mechanisms of acoustical oscillators using the example of synchronization of organ pipes N2 - In dieser Arbeit werden nichtlineare Kopplungsmechanismen von akustischen Oszillatoren untersucht, die zu Synchronisation führen können. Aufbauend auf die Fragestellungen vorangegangener Arbeiten werden mit Hilfe theoretischer und experimenteller Studien sowie mit Hilfe numerischer Simulationen die Elemente der Tonentstehung in der Orgelpfeife und die Mechanismen der gegenseitigen Wechselwirkung von Orgelpfeifen identifiziert. Daraus wird erstmalig ein vollständig auf den aeroakustischen und fluiddynamischen Grundprinzipien basierendes nichtlinear gekoppeltes Modell selbst-erregter Oszillatoren für die Beschreibung des Verhaltens zweier wechselwirkender Orgelpfeifen entwickelt. Die durchgeführten Modellrechnungen werden mit den experimentellen Befunden verglichen. Es zeigt sich, dass die Tonentstehung und die Kopplungsmechanismen von Orgelpfeifen durch das entwickelte Oszillatormodell in weiten Teilen richtig beschrieben werden. Insbesondere kann damit die Ursache für den nichtlinearen Zusammenhang von Kopplungsstärke und Synchronisation des gekoppelten Zwei-Pfeifen Systems, welcher sich in einem nichtlinearen Verlauf der Arnoldzunge darstellt, geklärt werden. Mit den gewonnenen Erkenntnissen wird der Einfluss des Raumes auf die Tonentstehung bei Orgelpfeifen betrachtet. Dafür werden numerische Simulationen der Wechselwirkung einer Orgelpfeife mit verschiedenen Raumgeometrien, wie z. B. ebene, konvexe, konkave, und gezahnte Geometrien, exemplarisch untersucht. Auch der Einfluss von Schwellkästen auf die Tonentstehung und die Klangbildung der Orgelpfeife wird studiert. In weiteren, neuartigen Synchronisationsexperimenten mit identisch gestimmten Orgelpfeifen, sowie mit Mixturen wird die Synchronisation für verschiedene, horizontale und vertikale Pfeifenabstände in der Ebene der Schallabstrahlung, untersucht. Die dabei erstmalig beobachteten räumlich isotropen Unstetigkeiten im Schwingungsverhalten der gekoppelten Pfeifensysteme, deuten auf abstandsabhängige Wechsel zwischen gegen- und gleichphasigen Sychronisationsregimen hin. Abschließend wird die Möglichkeit dokumentiert, das Phänomen der Synchronisation zweier Orgelpfeifen durch numerische Simulationen, also der Behandlung der kompressiblen Navier-Stokes Gleichungen mit entsprechenden Rand- und Anfangsbedingungen, realitätsnah abzubilden. Auch dies stellt ein Novum dar. N2 - In this work non-linear coupling mechanisms in acoustic oscillator systems are examined which can lead to synchronization phenomena. This mechanisms are investigated in particular on organ pipes. Building up on the questions of preceding works the elements of the sound generation are identified using detailed experimental and theoretical studies, as well as numerical simulations. Furthermore the organ pipes interaction mechanisms of the mutual coupling are developed. This leads to a non-linear coupled oscillator model which is developed on the aeroacoustical and fluiddynamical first principles. The carried out model calculations are compared to the experimental results from preceding works. It appears that the sound generation and the coupling mechanisms are properly described by the developed nonlinear coupled model of self-sustained oscillators. In particular the cause can be cleared with it for the non-linear edges of the Arnold tongue of the coupled two-pipe system. With the new knowledge the influence of various space geometries on the sound generation of organ pipes is investigated. With numerical simulations the interaction of an organ pipe and different space geometries, like plane, convex, concave, and ridged geometry is studied. Also the influence of so called swell boxes on the sound generation and the sound pattern of the organ pipe is studied. In further new synchronization experiments with precisely equally tuned pairs of organ pipes, as well as with mixtures the synchronization is examined for various grids of horizontal and vertical pipe distances in the 2D-plane of sound radiation. The spatial discontinuities observed in the oscillation behaviour of the coupled pipe systems, point to changes between anti-phase and in-phase regimes of sychronization depending on pipes distances. Finally the possibility is documented to describe the phenomenon of the synchronization of two organ pipes realisticaly by solving the compressible Navier-Stokes equations numerically. KW - Synchronisation KW - Orgelpfeifen KW - Simulation KW - Experiment KW - Modell KW - synchronization KW - organ pipes KW - simulation KW - experiment KW - model Y1 - 2014 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-71975 ER - TY - JOUR A1 - Cherstvy, Andrey G. A1 - Metzler, Ralf T1 - Nonergodicity, fluctuations, and criticality in heterogeneous diffusion processes JF - Physical review : E, Statistical, nonlinear and soft matter physics N2 - We study the stochastic behavior of heterogeneous diffusion processes with the power-law dependence D(x) similar to vertical bar x vertical bar(alpha) of the generalized diffusion coefficient encompassing sub- and superdiffusive anomalous diffusion. Based on statistical measures such as the amplitude scatter of the time-averaged mean-squared displacement of individual realizations, the ergodicity breaking and non-Gaussianity parameters, as well as the probability density function P(x, t), we analyze the weakly nonergodic character of the heterogeneous diffusion process and, particularly, the degree of irreproducibility of individual realizations. As we show, the fluctuations between individual realizations increase with growing modulus vertical bar alpha vertical bar of the scaling exponent. The fluctuations appear to diverge when the critical value alpha = 2 is approached, while for even larger alpha the fluctuations decrease, again. At criticality, the power-law behavior of the mean-squared displacement changes to an exponentially fast growth, and the fluctuations of the time-averaged mean-squared displacement do not converge for increasing number of realizations. From a systematic comparison we observe some striking similarities of the heterogeneous diffusion process with the familiar subdiffusive continuous time random walk process with power-law waiting time distribution and diverging characteristic waiting time. Y1 - 2014 U6 - https://doi.org/10.1103/PhysRevE.90.012134 SN - 1539-3755 SN - 1550-2376 VL - 90 IS - 1 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Foertig, Alexander A1 - Kniepert, Juliane A1 - Gluecker, Markus A1 - Brenner, Thomas J. K. A1 - Dyakonov, Vladimir A1 - Neher, Dieter A1 - Deibel, Carsten T1 - Nongeminate and geminate recombination in PTB7: PCBM solar cells JF - Advanced functional materials KW - organic semiconductors KW - organic solar cells KW - conjugated polymers KW - charge carrier recombination Y1 - 2014 U6 - https://doi.org/10.1002/adfm.201302134 SN - 1616-301X SN - 1616-3028 VL - 24 IS - 9 SP - 1306 EP - 1311 PB - Wiley-VCH CY - Weinheim ER - TY - JOUR A1 - Lepri, Stefano A1 - Pikovskij, Arkadij T1 - Nonreciprocal wave scattering on nonlinear string-coupled oscillators JF - Chaos : an interdisciplinary journal of nonlinear science N2 - We study scattering of a periodic wave in a string on two lumped oscillators attached to it. The equations can be represented as a driven (by the incident wave) dissipative (due to radiation losses) system of delay differential equations of neutral type. Nonlinearity of oscillators makes the scattering non-reciprocal: The same wave is transmitted differently in two directions. Periodic regimes of scattering are analyzed approximately, using amplitude equation approach. We show that this setup can act as a nonreciprocal modulator via Hopf bifurcations of the steady solutions. Numerical simulations of the full system reveal nontrivial regimes of quasiperiodic and chaotic scattering. Moreover, a regime of a "chaotic diode," where transmission is periodic in one direction and chaotic in the opposite one, is reported. (C) 2014 AIP Publishing LLC. Y1 - 2014 U6 - https://doi.org/10.1063/1.4899205 SN - 1054-1500 SN - 1089-7682 VL - 24 IS - 4 PB - American Institute of Physics CY - Melville ER - TY - JOUR A1 - Nezhadhaghighi, M. Ghasemi A1 - Chechkin, Aleksei V. A1 - Metzler, Ralf T1 - Numerical approach to unbiased and driven generalized elastic model JF - The journal of chemical physics : bridges a gap between journals of physics and journals of chemistr N2 - From scaling arguments and numerical simulations, we investigate the properties of the generalized elastic model (GEM) that is used to describe various physical systems such as polymers, membranes, single-file systems, or rough interfaces. We compare analytical and numerical results for the subdiffusion exponent beta characterizing the growth of the mean squared displacement <(delta h)(2)> of the field h described by the GEM dynamic equation. We study the scaling properties of the qth order moments with time, finding that the interface fluctuations show no intermittent behavior. We also investigate the ergodic properties of the process h in terms of the ergodicity breaking parameter and the distribution of the time averaged mean squared displacement. Finally, we study numerically the driven GEM with a constant, localized perturbation and extract the characteristics of the average drift for a tagged probe. Y1 - 2014 U6 - https://doi.org/10.1063/1.4858425 SN - 0021-9606 SN - 1089-7690 VL - 140 IS - 2 PB - American Institute of Physics CY - Melville ER - TY - JOUR A1 - Acciari, V. A. A1 - Arlen, T. A1 - Aune, T. A1 - Benbow, W. A1 - Bird, R. A1 - Bouvier, A. A1 - Bradbury, S. M. A1 - Buckley, J. H. A1 - Bugaev, V. A1 - de la Calle Perez, I. A1 - Carter-Lewis, D. A. A1 - Cesarini, A. A1 - Ciupik, L. A1 - Collins-Hughes, E. A1 - Connolly, M. P. A1 - Cui, W. A1 - Duke, C. A1 - Dumm, J. A1 - Falcone, A. A1 - Federici, Simone A1 - Fegan, D. J. A1 - Fegan, S. J. A1 - Finley, J. P. A1 - Finnegan, G. A1 - Fortson, L. A1 - Gaidos, J. A1 - Galante, N. A1 - Gall, D. A1 - Gibbs, K. A1 - Gillanders, G. H. A1 - Griffin, S. A1 - Grube, J. A1 - Gyuk, G. A1 - Hanna, D. A1 - Horan, D. A1 - Humensky, T. B. A1 - Kaaret, P. A1 - Kertzman, M. A1 - Khassen, Y. A1 - Kieda, D. A1 - Krawczynski, H. A1 - Krennrich, F. A1 - Lang, M. J. A1 - McEnery, J. E. A1 - Madhavan, A. S. A1 - Moriarty, P. A1 - Nelson, T. A1 - Ong, R. A. A1 - Orr, M. A1 - Otte, A. N. A1 - Perkins, J. S. A1 - Petry, D. A1 - Pichel, A. A1 - Pohl, M. A1 - Quinn, J. A1 - Ragan, K. A1 - Reynolds, T. A1 - Roache, E. A1 - Rovero, A. A1 - Schroedter, M. A1 - Sembroski, G. H. A1 - Smith, A. A1 - Telezhinsky, Igor O. A1 - Theiling, M. A1 - Toner, J. A1 - Tyler, J. A1 - Varlotta, A. A1 - Vivier, M. A1 - Wakely, S. P. A1 - Ward, J. E. A1 - Weekes, T. C. A1 - Weinstein, A. A1 - Welsing, R. A1 - Williams, D. A. A1 - Wissel, S. T1 - Observation of Markarian 421 in TeV gamma rays over a 14-year time span JF - Astroparticle physics N2 - The variability of the blazar Markarian 421 in TeV gamma rays over a 14-year time period has been explored with the Whipple 10 m telescope. It is shown that the dynamic range of its flux variations is large and similar to that in X-rays. A correlation between the X-ray and TeV energy bands is observed during some bright flares and when the complete data sets are binned on long timescales. The main database consists of 878.4 h of observation with the Whipple telescope, spread over 783 nights. The peak energy response of the telescope was 400 GeV with 20% uncertainty. This is the largest database of any TeV-emitting active galactic nucleus (AGN) and hence was used to explore the variability profile of Markarian 421. The tithe-averaged flux from Markarian 421 over this period was 0.446 +/- 0.008 Crab flux units. The flux exceeded 10 Crab flux units on three separate occasions. For the 2000-2001 season the average flux reached 1.86 Crab units, while in the 1996-1997 season the average flux was only 0.23 Crab units. KW - AGN KW - TeV gamma rays KW - Markarian 421 Y1 - 2014 U6 - https://doi.org/10.1016/j.astropartphys.2013.10.004 SN - 0927-6505 SN - 1873-2852 VL - 54 SP - 1 EP - 10 PB - Elsevier CY - Amsterdam ER - TY - JOUR A1 - Danehkar, A. A1 - Todt, Helge Tobias A1 - Ercolano, B. A1 - Kniazev, A. Y. T1 - Observations and three-dimensional photoionization modelling of the Wolf-Rayet planetary nebula Abell 48(star) JF - Monthly notices of the Royal Astronomical Society N2 - Recent observations reveal that the central star of the planetary nebula Abell 48 exhibits spectral features similar to massive nitrogen-sequence Wolf-Rayet stars. This raises a pertinent question, whether it is still a planetary nebula or rather a ring nebula of a massive star. In this study, we have constructed a three-dimensional photoionization model of Abell 48, constrained by our new optical integral field spectroscopy. An analysis of the spatially resolved velocity distributions allowed us to constrain the geometry of Abell 48. We used the collisionally excited lines to obtain the nebular physical conditions and ionic abundances of nitrogen, oxygen, neon, sulphur and argon, relative to hydrogen. We also determined helium temperatures and ionic abundances of helium and carbon from the optical recombination lines. We obtained a good fit to the observations for most of the emission-line fluxes in our photoionization model. The ionic abundances deduced from our model are in decent agreement with those derived by the empirical analysis. However, we notice obvious discrepancies between helium temperatures derived from the model and the empirical analysis, as overestimated by our model. This could be due to the presence of a small fraction of cold metal-rich structures, which were not included in our model. It is found that the observed nebular line fluxes were best reproduced by using a hydrogen-deficient expanding model atmosphere as the ionizing source with an effective temperature of T-eff = 70 kK and a stellar luminosity of L-star = 5500 L-circle dot, which corresponds to a relatively low-mass progenitor star (similar to 3 M-circle dot) rather than a massive Pop I star. KW - stars: Wolf-Rayet KW - ISM: abundances KW - planetary nebulae: individual: Abell 48 Y1 - 2014 U6 - https://doi.org/10.1093/mnras/stu203 SN - 0035-8711 SN - 1365-2966 VL - 439 IS - 4 SP - 3605 EP - 3615 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Aliu, E. A1 - Aune, T. A1 - Behera, B. A1 - Beilicke, M. A1 - Benbow, W. A1 - Berger, K. A1 - Bird, R. A1 - Buckley, J. H. A1 - Bugaev, V. A1 - Cardenzana, J. V. A1 - Cerruti, M. A1 - Chen, X. 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 - Fortin, 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 - Kargaltsev, Oleg 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 - McCann, A. A1 - Moriarty, P. A1 - Mukherjee, R. A1 - Nieto, D. A1 - Ong, R. A. A1 - Otte, A. N. A1 - Pandel, D. A1 - Perkins, J. S. A1 - Pohl, Manuela 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 - Skole, C. 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 - Welsing, R. A1 - Williams, D. A. A1 - Zitzer, B. T1 - Observations of the unidentified gamm-ray source TeV J2032+4130 BY Veritas JF - The astrophysical journal : an international review of spectroscopy and astronomical physics KW - gamma rays: general KW - pulsars: individual (PSR J2032+4127) Y1 - 2014 U6 - https://doi.org/10.1088/0004-637X/783/1/16 SN - 0004-637X SN - 1538-4357 VL - 783 IS - 1 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Reindl, Nicole A1 - Rauch, Thomas A1 - Werner, Klaus A1 - Kruk, J. W. A1 - Todt, Helge Tobias T1 - On helium-dominated stellar evolution: the mysterious role of the O(He)-type stars JF - Astronomy and astrophysics : an international weekly journal N2 - Context. About a quarter of all post-asymptotic giant branch (AGB) stars are hydrogen-deficient. Stellar evolutionary models explain the carbon-dominated H-deficient stars by a (very) late thermal pulse scenario where the hydrogen-rich envelope is mixed with the helium-rich intershell layer. Depending on the particular time at which the final flash occurs, the entire hydrogen envelope may be burned. In contrast, helium-dominated post-AGB stars and their evolution are not yet understood. Aims. A small group of very hot, helium-dominated stars is formed by O(He)-type stars. A precise analysis of their photospheric abundances will establish constraints to their evolution. Methods. We performed a detailed spectral analysis of ultraviolet and optical spectra of four O(He) stars by means of state-of-the-art non-LTE model-atmosphere techniques. Results. We determined effective temperatures, surface gravities, and the abundances of H, He, C, N, O, F, Ne, Si, P, S, Ar, and Fe. By deriving upper limits for the mass-loss rates of the O(He) stars, we found that they do not exhibit enhanced mass-loss. The comparison with evolutionary models shows that the status of the O(He) stars remains uncertain. Their abundances match predictions of a double helium white dwarf (WD) merger scenario, suggesting that they might be the progeny of the compact and of the luminous helium-rich sdO-type stars. The existence of planetary nebulae that do not show helium enrichment around every other O(He) star precludes a merger origin for these stars. These stars must have formed in a different way, for instance via enhanced mass-loss during their post-AGB evolution or a merger within a common-envelope (CE) of a CO-WD and a red giant or AGB star. Conclusions. A helium-dominated stellar evolutionary sequence exists that may be fed by different types of mergers or CE scenarios. It appears likely that all these pass through the O(He) phase just before they become WDs. KW - stars: AGB and post-AGB KW - stars: evolution KW - stars: fundamental parameters KW - stars: abundances Y1 - 2014 U6 - https://doi.org/10.1051/0004-6361/201423498 SN - 0004-6361 SN - 1432-0746 VL - 566 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Mkrtchian, Vanik E. A1 - Henkel, Carsten T1 - On non-equilibrium photon distributions in the Casimir effect JF - Annalen der Physik N2 - The electromagnetic field in a typical geometry of the Casimir effect is described in the Schwinger-Keldysh formalism. The main result is the photon distribution function (Keldysh Green function) in any stationary state of the field. A two-plate geometry with a sliding interface in local equilibrium is studied in detail, and full agreement with the results of Rytov fluctuation electrodynamics is found. KW - Casimir effect KW - van der Waals interaction KW - quantum friction KW - nonequilibrium electrodynamics of nanosystems Y1 - 2014 U6 - https://doi.org/10.1002/andp.201300135 SN - 0003-3804 SN - 1521-3889 VL - 526 IS - 1-2 SP - 87 EP - 101 PB - Wiley-VCH CY - Weinheim ER - TY - JOUR A1 - Albrecht, Steve A1 - Vandewal, Koen A1 - Tumbleston, John R. A1 - Fischer, Florian S. U. A1 - Douglas, Jessica D. A1 - Frechet, Jean M. J. A1 - Ludwigs, Sabine A1 - Ade, Harald W. A1 - Salleo, Alberto A1 - Neher, Dieter T1 - On the efficiency of charge transfer state splitting in polymer: Fullerene solar cells JF - Advanced materials KW - organic solar cells KW - charge generation KW - geminate recombination KW - charge transfer states KW - driving force KW - excess energy KW - morphology KW - spectroelectrochemistry Y1 - 2014 U6 - https://doi.org/10.1002/adma.201305283 SN - 0935-9648 SN - 1521-4095 VL - 26 IS - 16 SP - 2533 EP - 2539 PB - Wiley-VCH CY - Weinheim ER - TY - THES A1 - Conrad, Claudia T1 - Open cluster groups and complexes T1 - Gruppen und Komplexe offener Sternhaufen N2 - It is generally agreed upon that stars typically form in open clusters and stellar associations, but little is known about the structure of the open cluster system. Do open clusters and stellar associations form isolated or do they prefer to form in groups and complexes? Open cluster groups and complexes could verify star forming regions to be larger than expected, which would explain the chemical homogeneity over large areas in the Galactic disk. They would also define an additional level in the hierarchy of star formation and could be used as tracers for the scales of fragmentation in giant molecular clouds? Furthermore, open cluster groups and complexes could affect Galactic dynamics and should be considered in investigations and simulations on the dynamical processes, such as radial migration, disc heating, differential rotation, kinematic resonances, and spiral structure. In the past decade there were a few studies on open cluster pairs (de La Fuente Marcos & de La Fuente Marcos 2009a,b,c) and on open cluster groups and complexes (Piskunov et al. 2006). The former only considered spatial proximity for the identification of the pairs, while the latter also required tangential velocities to be similar for the members. In this work I used the full set of 6D phase-space information to draw a more detailed picture on these structures. For this purpose I utilised the most homogeneous cluster catalogue available, namely the Catalogue of Open Cluster Data (COCD; Kharchenko et al. 2005a,b), which contains parameters for 650 open clusters and compact associations, as well as for their uniformly selected members. Additional radial velocity (RV) and metallicity ([M/H]) information on the members were obtained from the RAdial Velocity Experiment (RAVE; Steinmetz et al. 2006; Kordopatis et al. 2013) for 110 and 81 clusters, respectively. The RAVE sample was cleaned considering quality parameters and flags provided by RAVE (Matijevič et al. 2012; Kordopatis et al. 2013). To ensure that only real members were included for the mean values, also the cluster membership, as provided by Kharchenko et al. (2005a,b), was considered for the stars cross-matched in RAVE. 6D phase-space information could be derived for 432 out of the 650 COCD objects and I used an adaption of the Friends-of-Friends algorithm, as used in cosmology, to identify potential groupings. The vast majority of the 19 identified groupings were pairs, but I also found four groups of 4-5 members and one complex with 15 members. For the verification of the identified structures, I compared the results to a randomly selected subsample of the catalogue for the Milky Way global survey of Star Clusters (MWSC; Kharchenko et al. 2013), which became available recently, and was used as reference sample. Furthermore, I implemented Monte-Carlo simulations with randomised samples created from two distinguished input distributions for the spatial and velocity parameters. On the one hand, assuming a uniform distribution in the Galactic disc and, on the other hand, assuming the COCD data distributions to be representative for the whole open cluster population. The results suggested that the majority of identified pairs are rather by chance alignments, but the groups and the complex seemed to be genuine. A comparison of my results to the pairs, groups and complexes proposed in the literature yielded a partial overlap, which was most likely because of selection effects and different parameters considered. This is another verification for the existence of such structures. The characteristics of the found groupings favour that members of an open cluster grouping originate from a common giant molecular cloud and formed in a single, but possibly sequential, star formation event. Moreover, the fact that the young open cluster population showed smaller spatial separations between nearest neighbours than the old cluster population indicated that the lifetime of open cluster groupings is most likely comparable to that of the Galactic open cluster population itself. Still even among the old open clusters I could identify groupings, which suggested that the detected structure could be in some cases more long lived as one might think. In this thesis I could only present a pilot study on structures in the Galactic open cluster population, since the data sample used was highly incomplete. For further investigations a far more complete sample would be required. One step in this direction would be to use data from large current surveys, like SDSS, RAVE, Gaia-ESO and VVV, as well as including results from studies on individual clusters. Later the sample can be completed by data from upcoming missions, like Gaia and 4MOST. Future studies using this more complete open cluster sample will reveal the effect of open cluster groupings on star formation theory and their significance for the kinematics, dynamics and evolution of the Milky Way, and thereby of spiral galaxies. N2 - Es ist weithin anerkannt, dass Sterne typischerweise in offenen Sternenhaufen und Sternassoziationen entstehen, dennoch ist wenig über Strukturen in diesem System der offenen Sternhaufen bekannt. Entstehen offenen Sternhaufen und Sternassoziationen isoliert oder entstehen sie bevorzugt in Gruppen und Komplexen? Gruppen und Komplexe von offenen Sternhaufen könnten bestätigen, dass Sternentstehungsregionen größer sind als erwartet, was die Homogenität der chemischen Zusammensetzung über weite Areale in der galaktischen Scheibe erklären würde. Sie würden auch eine weitere Stufe in der Hierarchie der Sternentstehung definieren und könnten als Indikatoren für die Skalen der Fragmentierung in Riesenmolekülwolken dienen. Des Weiteren könnten Gruppen und Komplexe von offenen Sternhaufen die Dynamik unserer Galaxis beeinflussen und sollten in Untersuchungen und Simulationen von dynamischen Prozessen, wie radiale Migration, kinematische Aufheizung der Scheibe, differentielle Rotation, kinematische Resonanzen und der Spiralstruktur, miteinbezogen werden. In den vergangenen Jahrzehnten gab es einigen Studien zu Paaren von offenen Sternhaufen (de La Fuente Marcos & de La Fuente Marcos 2009a,b,c) sowie zu Gruppen und Komplexen von offenen Sternhaufen (Piskunov et al. 2006). Erstere betrachteten ausschließlich räumliche Nähe für die Identifizierung der Paare, während letztere auch ähnliche tangentiale Geschwindigkeiten für die Mitglieder verlangten. In dieser Arbeit nutzte ich den kompletten Satz an 6D-Phasenrauminformationen, um ein vollständigeres Bild dieser Strukturen zu erstellen. Aus diesem Grund habe ich den homogensten Sternhaufenkatalog verwendet, der zu dieser Zeit verfügbar war, nämlich den Catalogue of Open Cluster Data (COCD; Kharchenko et al. 2005a,b), welcher Parameter für 650 offene Sternhaufen und Sternassoziationen, sowie deren einheitlich ausgewählte Mitglieder, enthält. Weitere Radialgeschwindigkeits- (RV) und Metallizitätsinformationen ([M/H]) für die Sternhaufenmitglieder wurden mit Hilfe des RAdial Velocity Experiment (RAVE; Steinmetz et al. 2006; Kordopatis et al. 2013) für 110 beziehungsweise 81 Haufen bestimmt. Der RAVE-Datensatz wurde mit Hilfe von Qualitätsparametern aus RAVE (Matijevič et al. 2012; Kordopatis et al. 2013) gereinigt. Um sicherzustellen, dass nur echte Mitglieder für die Mittelwertbestimmung betrachtet wurden, wurde auch die Haufenmitgliedschaft, wie von Kharchenko et al. (2005a,b) bereitgestellt, für die in RAVE identifizierten Sterne miteinbezogen. 6D-Phasenrauminformationen konnten für 432 der 650 COCD Objekte bestimmt werden und ich habe eine angepasste Variante des Friends-of-Friends Algorithmus genutzt, der in der Kosmologie verwendet wird, um potenzielle Gruppierungen zu identifizieren. Der überwiegende Teil der 19 identifizierten Gruppierungen waren Paare, ich habe aber auch vier Gruppen mit 4-5 Mitgliedern und einen Komplex mit 15 Mitgliedern gefunden. Für die Bestätigung der identifizierten Strukturen, verglich ich die Ergebnisse mit einem zufällig ausgewählten Datensatz aus dem Milky Way global survey of Star Clusters (MWSC; Kharchenko et al. 2013), der kürzlich erst zur Verfügung gestellt wurde und hier als Vergleichsdatensatz verwendet wurde. Des Weiteren, habe ich Monte-Carlo Simulationen mit zufälligen Datensätzen implementiert, die anhand von zwei unterschiedlichen Varianten für die Ausgangsverteilungen der räumlichen und Geschwindigkeitsparameter generiert wurden. Zum Einen unter der Annahme einer gleichmäßigen Verteilung in der galaktischen Scheibe und zum Anderen unter der Annahme, dass die Datenverteilungen im COCD repräsentativ sind für die gesamte Population der offenen Sternhaufen. Die Ergebnisse deuteten darauf hin, dass die Mehrheit der identifizierten Paare eher zufällige Anordnungen sind, aber die Gruppen und der Komplex schienen echt zu sein. Ein Vergleich meiner Ergebnisse mit den in der Literatur vorgeschlagenen Paaren, Gruppen und Komplexen ergab eine teilweise Überschneidung, die höchstwahrscheinlich durch Auswahleffekte und die Verwendung unterschiedlicher Parameter bedingt war. Dies ist eine weitere Bestätigung für die Existenz solcher Strukturen. Die Eigenschaften der gefundenen Gruppierungen bevorzugen, dass die Mitglieder einer Gruppierung von offenen Sternhaufen aus einer gemeinsamen Riesenmolekülwolke stammen und in einem Sternentstehungsereignis geformt wurden, das möglicherweise auch sequenziell ablief. Außerdem zeigte die junge Population der offenen Sternhaufen kleinere räumliche Abstände zwischen den nächsten Nachbarn als die alte Haufenpopulation, was darauf hindeutet, dass die Lebenszeit von Gruppierungen von offenen Sternhaufen vergleichbar ist mit der für die Population galaktischer offener Sternhaufen selbst. Dennoch wurden auch unter den alten offenen Sternhaufen Gruppierungen identifiziert, was andeutete, dass die gefundenen Strukturen doch in einigen Fällen langlebiger ist als man denken könnte. In dieser Doktorarbeit konnte ich nur eine Pilotstudie zu Strukturen in der Population der galaktischen offenen Sternhaufen präsentieren, da der verwendete Datensatz höchst unvollständig war. Für zukünftige Untersuchungen wäre ein deutlich vollständigerer Datensatz notwendig. Ein Schritt in diese Richtung wäre die Verwendung von Daten aus großen momentan verfügbaren Beobachtungskampagnen, wie dem SDSS, RAVE, Gaia-ESO und dem VVV, sowie das miteinbeziehen der Ergebnisse von Studien an einzelnen offenen Sternhaufen. Später könnte dieser Datensatz durch die Verwendung von Daten aus kommenden Missionen, wie Gaia und 4MOST, komplettiert werden. Zukünftige Studien mit einem vollständigeren Datensatz werden den Einfluss von Gruppierungen von offenen Sternhaufen für die Sternentstehungstheorie und ihre Bedeutung für die Kinematik, Dynamik und Entwicklung der Milchstraße, und damit auch für andere Spiralgalaxien, enträtseln. KW - open clusters and stellar associations KW - stellar populations KW - offene Sternhaufen und stellare Assoziationen KW - Sternpopulationen Y1 - 2014 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-77605 ER - TY - GEN A1 - Eschenlohr, Andrea A1 - Battiato, Mario A1 - Maldonado, P. A1 - Pontius, N. A1 - Kachel, T. A1 - Holldack, K. A1 - Mitzner, Rolf A1 - Föhlisch, Alexander A1 - Oppeneer, P. M. A1 - Stamm, Christian T1 - Optical excitation of thin magnetic layers in multilayer structures Reply T2 - Nature materials Y1 - 2014 U6 - https://doi.org/10.1038/nmat3851 SN - 1476-1122 SN - 1476-4660 VL - 13 IS - 2 SP - 102 EP - 103 PB - Nature Publ. Group CY - London ER - TY - JOUR A1 - Proctor, Christopher M. A1 - Albrecht, Steve A1 - Kuik, Martijn A1 - Neher, Dieter A1 - Thuc-Quyen Nguyen, T1 - Overcoming geminate recombination and enhancing extraction in solution-processed small molecule solar cells JF - dvanced energy materials Y1 - 2014 U6 - https://doi.org/10.1002/aenm.201400230 SN - 1614-6832 SN - 1614-6840 VL - 4 IS - 10 PB - Wiley-VCH CY - Weinheim ER - TY - JOUR A1 - Moule, Adam J. A1 - Neher, Dieter A1 - Turner, Sarah T. ED - Ludwigs, S T1 - P3HT-Based solar cells: structural properties and photovoltaic performance JF - Advances in Polymer Science JF - Advances in Polymer Science N2 - Each year we are bombarded with B.Sc. and Ph.D. applications from students that want to improve the world. They have learned that their future depends on changing the type of fuel we use and that solar energy is our future. The hope and energy of these young people will transform future energy technologies, but it will not happen quickly. Organic photovoltaic devices are easy to sketch, but the materials, processing steps, and ways of measuring the properties of the materials are very complicated. It is not trivial to make a systematic measurement that will change the way other research groups think or practice. In approaching this chapter, we thought about what a new researcher would need to know about organic photovoltaic devices and materials in order to have a good start in the subject. Then, we simplified that to focus on what a new researcher would need to know about poly-3-hexylthiophene: phenyl-C61-butyric acid methyl ester blends (P3HT: PCBM) to make research progress with these materials. This chapter is by no means authoritative or a compendium of all things on P3HT: PCBM. We have selected to explain how the sample fabrication techniques lead to control of morphology and structural features and how these morphological features have specific optical and electronic consequences for organic photovoltaic device applications. KW - Free carrier generation KW - Non-geminate recombination KW - Organic solar cells Y1 - 2014 SN - 978-3-662-45145-8; 978-3-662-45144-1 U6 - https://doi.org/10.1007/12_2014_289 SN - 0065-3195 VL - 265 SP - 181 EP - 232 PB - Springer CY - Berlin ER - TY - JOUR A1 - Cherstvy, Andrey G. A1 - Chechkin, Aleksei V. A1 - Metzler, Ralf T1 - Particle invasion, survival, and non-ergodicity in 2D diffusion processes with space-dependent diffusivity JF - Soft matter N2 - We study the thermal Markovian diffusion of tracer particles in a 2D medium with spatially varying diffusivity D(r), mimicking recently measured, heterogeneous maps of the apparent diffusion coefficient in biological cells. For this heterogeneous diffusion process (HDP) we analyse the mean squared displacement (MSD) of the tracer particles, the time averaged MSD, the spatial probability density function, and the first passage time dynamics from the cell boundary to the nucleus. Moreover we examine the non-ergodic properties of this process which are important for the correct physical interpretation of time averages of observables obtained from single particle tracking experiments. From extensive computer simulations of the 2D stochastic Langevin equation we present an in-depth study of this HDP. In particular, we find that the MSDs along the radial and azimuthal directions in a circular domain obey anomalous and Brownian scaling, respectively. We demonstrate that the time averaged MSD stays linear as a function of the lag time and the system thus reveals a weak ergodicity breaking. Our results will enable one to rationalise the diffusive motion of larger tracer particles such as viruses or submicron beads in biological cells. Y1 - 2014 U6 - https://doi.org/10.1039/c3sm52846d SN - 1744-683X SN - 1744-6848 VL - 10 IS - 10 SP - 1591 EP - 1601 PB - Royal Society of Chemistry CY - Cambridge ER - TY - JOUR A1 - Zakrevskyy, Yuriy A1 - Titov, Evgenii A1 - Lomadze, Nino A1 - Santer, Svetlana T1 - Phase diagrams of DNA-photosensitive surfactant complexes: Effect of ionic strength and surfactant structure JF - The journal of chemical physics : bridges a gap between journals of physics and journals of chemistr N2 - Realization of all-optically controlled and efficient DNA compaction is the major motivation in the study of interactions between DNA and photosensitive surfactants. In this article, using recently published approach of phase diagram construction [Y. Zakrevskyy, P. Cywinski, M. Cywinska, J. Paasche, N. Lomadze, O. Reich, H.-G. Lohmannsroben, and S. Santer, J. Chem. Phys. 140, 044907 (2014)], a strategy for substantial reduction of compaction agent concentration and simultaneous maintaining the light-induced decompaction efficiency is proposed. The role of ionic strength (NaCl concentration), as a very important environmental parameter, and surfactant structure (spacer length) on the changes of positions of phase transitions is investigated. Increase of ionic strength leads to increase of the surfactant concentration needed to compact DNA molecule. However, elongation of the spacer results to substantial reduction of this concentration. DNA compaction by surfactants with longer tails starts to take place in diluted solutions at charge ratios Z < 1 and is driven by azobenzene-aggregation compaction mechanism, which is responsible for efficient decompaction. Comparison of phase diagrams for different DNA-photosensitive surfactant systems allowed explanation and proposal of a strategy to overcome previously reported limitations of the light-induced decompaction for complexes with increasing surfactant hydrophobicity. (C) 2014 AIP Publishing LLC. Y1 - 2014 U6 - https://doi.org/10.1063/1.4899281 SN - 0021-9606 SN - 1089-7690 VL - 141 IS - 16 PB - American Institute of Physics CY - Melville ER - TY - JOUR A1 - Heuer, Axel A1 - Raabe, S. A1 - Menzel, Ralf T1 - Phase memory across two single-photon interferometers including wavelength conversion JF - Physical review : A, Atomic, molecular, and optical physics N2 - Spontaneous parametric down-conversion (SPDC) in a nonlinear crystal generates two single photons (signal and idler) with random phases. Thus, no first-order interference between them occurs. However, coherence can be induced in a cascaded setup of two crystals if, e.g., the idler modes of both crystals are aligned to be indistinguishable. Due to the effect of phase memory it is found that the first-order interference of the signal beams can be controlled by the phase delay between the pump beams. Even for pump photon delays much larger than the coherence length of the SPDC photons, the visibility is above 90%. The high visibilities reported here prove an almost perfect phase memory effect across the two interferometers for the pump and the signal photon modes. Y1 - 2014 U6 - https://doi.org/10.1103/PhysRevA.90.045803 SN - 1050-2947 SN - 1094-1622 VL - 90 IS - 4 PB - American Physical Society CY - College Park ER - TY - THES A1 - Holler, Markus T1 - Photon reconstruction for the H.E.S.S. 28 m telescope and analysis of Crab Nebula and galactic centre observations T1 - Photonrekonstruktion für das 28 m H.E.S.S. Teleskop und Analyse von Beobachtungen des Krebsnebels und des galaktischen Zentrums N2 - In the presented thesis, the most advanced photon reconstruction technique of ground-based γ-ray astronomy is adapted to the H.E.S.S. 28 m telescope. The method is based on a semi-analytical model of electromagnetic particle showers in the atmosphere. The properties of cosmic γ-rays are reconstructed by comparing the camera image of the telescope with the Cherenkov emission that is expected from the shower model. To suppress the dominant background from charged cosmic rays, events are selected based on several criteria. The performance of the analysis is evaluated with simulated events. The method is then applied to two sources that are known to emit γ-rays. The first of these is the Crab Nebula, the standard candle of ground-based γ-ray astronomy. The results of this source confirm the expected performance of the reconstruction method, where the much lower energy threshold compared to H.E.S.S. I is of particular importance. A second analysis is performed on the region around the Galactic Centre. The analysis results emphasise the capabilities of the new telescope to measure γ-rays in an energy range that is interesting for both theoretical and experimental astrophysics. The presented analysis features the lowest energy threshold that has ever been reached in ground-based γ-ray astronomy, opening a new window to the precise measurement of the physical properties of time-variable sources at energies of several tens of GeV. N2 - In der vorliegenden Dissertation wird die zur Zeit sensitivste Methode zur Photonrekonstruktion in der bodengebundenen Gammastrahlungsastronomie an das 28 m H.E.S.S. Teleskop angepasst. Die Analyse basiert auf einem semi-analytischen Modell von elektromagnetischen Teilchenschauern in der Erdatmosphäre. Die Rekonstruktion erfolgt durch den Vergleich des Bildes der Teleskopkamera mit der Tscherenkow-Emission, die mittels des Schauermodells berechnet wurde. Zur Verringerung des dominanten Untergrundes, der hauptsächlich durch Teilchen der geladenen kosmischen Strahlung hervorgerufen wird, werden Ereignisse anhand bestimmter Kriterien ausgewählt. Die Leistungsfähigkeit der Analyse wird unter Verwendung simulierter Ereignisse evaluiert. Die Methode wird anschließend auf zwei Gammastrahlungsquellen angewendet. Zuerst wird der Krebsnebel analysiert, die Standardkerze der bodengebundenen Gammastrahlungsastronomie. Die Resultate der Analyse des Krebsnebels bestätigen die bereits zuvor erwartete Leistungsfähigkeit der Rekonstruktionsmethode, wobei hier insbesondere die im Vergleich zu H.E.S.S. I stark verringerte Energieschwelle hervorzuheben ist. Als Zweites werden Beobachtungen der Region um das galaktische Zentrum ausgewertet. Die Analyseergebnisse dieser Daten unterstreichen die Fähigkeiten des neuen Teleskops zur Messung kosmischer Gammastrahlung in einem für die theoretische und experimentelle Astrophysik interessanten Energiebereich. Die vorgestellte Analyse besitzt die niedrigste Energieschwelle, die in der bodengebundenen Gammastrahlungsastronomie je erreicht wurde. Sie ermöglicht damit präzise Messungen der physikalischen Eigenschaften von zeitabhängigen Quellen im Energiebereich von 10 bis 100 GeV. KW - Gammastrahlungsastronomie KW - Rekonstruktionsmethoden KW - Datenanalyse KW - Krebsnebel KW - galaktisches Zentrum KW - gamma-ray astronomy KW - reconstruction methods KW - data analysis KW - Crab Nebula KW - galactic centre Y1 - 2014 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-72099 ER - TY - JOUR A1 - Yadavalli, Nataraja Sekhar A1 - Saphiannikova, Marina A1 - Santer, Svetlana T1 - Photosensitive response of azobenzene containing films towards pure intensity or polarization interference patterns JF - Applied physics letters N2 - In this paper, we report on differences in the response of photosensitive azobenzene containing films upon irradiation with the intensity or polarization interference patterns. Two materials are studied differing in the molecular weight: an azobenzene-containing polymer and a molecular glass formed from a much smaller molecule consisting of three connected azobenzene units. Topography changes occurring along with the changes in irradiation conditions are recorded using a homemade set-up combining an optical part for generation and shaping of interference patterns and an atomic force microscope for acquiring the kinetics of film deformation. In this way, we could reveal the unique behavior of photosensitive materials during the first few minutes of irradiation: the change in topography is initially driven by an increase in the azobenzene free volume along with the transcis isomerization, followed by the mass transport finally resulting in the surface relief grating. This study demonstrates the great potential of our setup to experimentally highlight puzzling processes governing the formation of surface relief gratings. (C) 2014 AIP Publishing LLC. Y1 - 2014 U6 - https://doi.org/10.1063/1.4891615 SN - 0003-6951 SN - 1077-3118 VL - 105 IS - 5 PB - American Institute of Physics CY - Melville ER - TY - JOUR A1 - Zakrevskyy, Yuriy A1 - Roxlau, Julian A1 - Brezesinski, Gerald A1 - Lomadze, Nino A1 - Santer, Svetlana T1 - Photosensitive surfactants: Micellization and interaction with DNA JF - The journal of chemical physics : bridges a gap between journals of physics and journals of chemistr N2 - Recently, photosensitive surfactants have re-attracted considerable attention. It has been shown that their association with oppositely charged biologically important polyelectrolytes, such as DNA or microgels, can be efficiently manipulated simply by light exposure. In this article, we investigate the self-assembly of photosensitive surfactants as well as their interactions with DNA by calorimetric and spectroscopic methods. Critical micelle concentration (CMC), standard micellization enthalpy, entropy, and Gibbs energy were determined in different conditions (ionic strengths and temperatures) for a series of cationic surfactants with an azobenzene group in their tail. It is shown, that aggregation forces of photosensitive units play an important role in the micellization giving the major contribution to the micellization enthalpy. The onset of the aggregation can be traced from shift of the absorption peak position in the UV-visible spectrum. Titration UV-visible spectroscopy is used as an alternative, simple, and sensitive approach to estimate CMC. The titration UV-visible spectroscopy was also employed to investigate interactions (CAC: critical aggregation concentration, precipitation, and colloidal stabilization) in the DNA-surfactant complex. Y1 - 2014 U6 - https://doi.org/10.1063/1.4862678 SN - 0021-9606 SN - 1089-7690 VL - 140 IS - 4 PB - American Institute of Physics CY - Melville ER - TY - BOOK A1 - Pohl, Martin T1 - Physik für alle T3 - Verdammt clever Y1 - 2014 SN - 978-3-527-41235-8 PB - Wiley CY - Hoboken ER - TY - JOUR A1 - Qiu, Xunlin A1 - Wirges, Werner A1 - Gerhard, Reimund T1 - Polarization and Hysteresis in Tubular-Channel Fluoroethylenepropylene-Copolymer Ferroelectrets JF - Ferroelectrics N2 - Polarization-vs.-applied-voltage hysteresis curves are recorded on tubular-channel fluoroethylene-propylene (FEP) copolymer ferroelectrets by means of a modified Sawyer-Tower circuit. Dielectric barrier discharges (DBDs) inside the cavities are triggered when the applied voltage is sufficiently high. During the DBDs, the cavities become man-made macroscopic dipoles which build up an effective polarization in the ferroelectret. Therefore, a phenomenological hysteresis curve is observed. From the hysteresis loop, the remanent polarization and the coercive field can be determined. Furthermore, the polarization can be related to the respective piezoelectric coefficient of the ferroelectret. The proposed method is easy to implement and is useful for characterization, further development and optimization of ferro- or piezoelectrets. KW - Ferroelectrets KW - piezoelectrets KW - tubular-channel polymer systems KW - dielectric barrier discharge (DBD) KW - fluoroethylenepropylene (FEP) copolymer KW - piezoelectricity-polarization relation Y1 - 2014 U6 - https://doi.org/10.1080/00150193.2014.964603 SN - 0015-0193 SN - 1563-5112 VL - 472 IS - 1 SP - 100 EP - 109 PB - Routledge, Taylor & Francis Group CY - Abingdon ER - TY - JOUR A1 - DiFlorio, Giuseppe A1 - Bründermann, Erik A1 - Yadavall, Nataraja Sekhar A1 - Santer, Svetlana A1 - Havenith, Martina T1 - Polarized 3D Raman and nanoscale near-field optical microscopy of optically inscribed surface relief gratings: chromophore orientation in azo-doped polymer films N2 - We have used polarized confocal Raman microspectroscopy and scanning near-field optical microscopy with a resolution of 60 nm to characterize photoinscribed grating structures of azobenzene doped polymer films on a glass support. Polarized Raman microscopy allowed determining the reorientation of the chromophores as a function of the grating phase and penetration depth of the inscribing laser in three dimensions. We found periodic patterns, which are not restricted to the surface alone, but appear also well below the surface in the bulk of the material. Near-field optical microscopy with nanoscale resolution revealed lateral two-dimensional optical contrast, which is not observable by atomic force and Raman microscopy. Y1 - 2014 UR - http://pubs.rsc.org/en/content/articlepdf/2014/sm/c3sm51787j U6 - https://doi.org/10.1039/c3sm51787j SN - 1744-683x ER - TY - JOUR A1 - Palyulin, Vladimir V. A1 - Ala-Nissila, Tapio A1 - Metzler, Ralf ED - Metzler, Ralf T1 - Polymer translocation: the first two decades and the recent diversification JF - Soft matter N2 - Probably no other field of statistical physics at the borderline of soft matter and biological physics has caused such a flurry of papers as polymer translocation since the 1994 landmark paper by Bezrukov, Vodyanoy, and Parsegian and the study of Kasianowicz in 1996. Experiments, simulations, and theoretical approaches are still contributing novel insights to date, while no universal consensus on the statistical understanding of polymer translocation has been reached. We here collect the published results, in particular, the famous–infamous debate on the scaling exponents governing the translocation process. We put these results into perspective and discuss where the field is going. In particular, we argue that the phenomenon of polymer translocation is non-universal and highly sensitive to the exact specifications of the models and experiments used towards its analysis. KW - solid-state nanopores KW - single-stranded-dna KW - posttranslational protein translocation KW - anomalous diffusion KW - monte-carlo KW - structured polynucleotides KW - dynamics simulation KW - equation approach KW - osmotic-pressure KW - membrane channel Y1 - 2014 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-76266 SN - 1744-683X VL - 45 IS - 10 SP - 9016 EP - 9037 PB - the Royal Society of Chemistry CY - Cambridge ER - TY - GEN A1 - Palyulin, Vladimir V. A1 - Ala-Nissila, Tapio A1 - Metzler, Ralf T1 - Polymer translocation: the first two decades and the recent diversification N2 - Probably no other field of statistical physics at the borderline of soft matter and biological physics has caused such a flurry of papers as polymer translocation since the 1994 landmark paper by Bezrukov, Vodyanoy, and Parsegian and the study of Kasianowicz in 1996. Experiments, simulations, and theoretical approaches are still contributing novel insights to date, while no universal consensus on the statistical understanding of polymer translocation has been reached. We here collect the published results, in particular, the famous–infamous debate on the scaling exponents governing the translocation process. We put these results into perspective and discuss where the field is going. In particular, we argue that the phenomenon of polymer translocation is non-universal and highly sensitive to the exact specifications of the models and experiments used towards its analysis. T3 - Zweitveröffentlichungen der Universität Potsdam : Mathematisch-Naturwissenschaftliche Reihe - 179 KW - solid-state nanopores KW - single-stranded-dna KW - posttranslational protein translocation KW - anomalous diffusion KW - monte-carlo KW - structured polynucleotides KW - dynamics simulation KW - equation approach KW - osmotic-pressure KW - membrane channel Y1 - 2014 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-76287 SP - 9016 EP - 9037 ER - TY - JOUR A1 - Palyulin, Vladimir V. A1 - Ala-Nissila, Tapio A1 - Metzler, Ralf T1 - Polymer translocation: the first two decades and the recent diversification JF - Soft matter N2 - Probably no other field of statistical physics at the borderline of soft matter and biological physics has caused such a flurry of papers as polymer translocation since the 1994 landmark paper by Bezrukov, Vodyanoy, and Parsegian and the study of Kasianowicz in 1996. Experiments, simulations, and theoretical approaches are still contributing novel insights to date, while no universal consensus on the statistical understanding of polymer translocation has been reached. We here collect the published results, in particular, the famous-infamous debate on the scaling exponents governing the translocation process. We put these results into perspective and discuss where the field is going. In particular, we argue that the phenomenon of polymer translocation is non-universal and highly sensitive to the exact specifications of the models and experiments used towards its analysis. Y1 - 2014 U6 - https://doi.org/10.1039/c4sm01819b SN - 1744-683X SN - 1744-6848 VL - 10 IS - 45 SP - 9016 EP - 9037 PB - Royal Society of Chemistry CY - Cambridge ER - TY - THES A1 - Schreck, Simon Frederik T1 - Potential energy surfaces, femtosecond dynamics and nonlinear X-Ray-Matter interactions from resonant inelastic soft x-Ray scattering Y1 - 2014 ER - TY - JOUR A1 - Yadavalli, Nataraja Sekhar A1 - Korolkov, Denis A1 - Moulin, Jean-Francois A1 - Krutyeva, Margarita A1 - Santer, Svetlana T1 - Probing opto-mechanical stresses within azobenzene-containing photosensitive polymer films by a thin metal film placed above JF - ACS applied materials & interfaces N2 - Azo-modified photosensitive polymers offer the interesting possibility to reshape bulk polymers and thin films by UV-irradiation while being in the solid glassy state. The polymer undergoes considerable mass transport under irradiation with a light interference pattern resulting in the formation of surface relief grating (SRG). The forces inscribing this SRG pattern into a thin film are hard to assess experimentally directly. In the current study, we are proposing a method to probe opto-mechanical stresses within polymer films by characterizing the mechanical response of thin metal films (10 nm) deposited on the photosensitive polymer. During irradiation, the metal film not only deforms along with the SRG formation but ruptures in a regular and complex manner. The morphology of the cracks differs strongly depending on the electrical field distribution in the interference pattern, even when the magnitude and the kinetics of the strain are kept constant. This implies a complex local distribution of the opto-mechanical stress along the topography grating. In addition, the neutron reflectivity measurements of the metal/polymer interface indicate the penetration of a metal layer within the polymer, resulting in a formation of a bonding layer that confirms the transduction of light-induced stresses in the polymer layer to a metal film. KW - surface relief grating KW - opto-mechanical stresses KW - bonding layer at the metal/polymer interface KW - rupturing of metal film KW - metal/multilayered graphene/polymer interfaces KW - azobenzene Y1 - 2014 U6 - https://doi.org/10.1021/am501870t SN - 1944-8244 VL - 6 IS - 14 SP - 11333 EP - 11340 PB - American Chemical Society CY - Washington ER - TY - JOUR A1 - Zamponi, Flavio A1 - Penfold, Thomas J. A1 - Nachtegaal, Maarten A1 - Luebcke, Andrea A1 - Rittmann, Jochen A1 - Milne, Chris J. A1 - Chergui, Majed A1 - van Bokhoven, Jeroen A. T1 - Probing the dynamics of plasmon-excited hexanethiol-capped gold nanoparticles by picosecond X-ray absorption spectroscopy JF - Physical chemistry, chemical physics : a journal of European Chemical Societies N2 - Picosecond X-ray absorption spectroscopy (XAS) is used to investigate the electronic and structural dynamics initiated by plasmon excitation of 1.8 nm diameter Au nanoparticles (NPs) functionalised with 1-hexanethiol. We show that 100 ps after photoexcitation the transient XAS spectrum is consistent with an 8% expansion of the Au-Au bond length and a large increase in disorder associated with melting of the NPs. Recovery of the ground state occurs with a time constant of similar to 1.8 ns, arising from thermalisation with the environment. Simulations reveal that the transient spectrum exhibits no signature of charge separation at 100 ps and allows us to estimate an upper limit for the quantum yield (QY) of this process to be <0.1. Y1 - 2014 U6 - https://doi.org/10.1039/c4cp03301a SN - 1463-9076 SN - 1463-9084 VL - 16 IS - 42 SP - 23157 EP - 23163 PB - Royal Society of Chemistry CY - Cambridge ER - TY - JOUR A1 - Yin, Zhong A1 - Rajkovic, Ivan A1 - Kubicek, Katharina A1 - Quevedo, Wilson A1 - Pietzsch, Annette A1 - Wernet, Philippe A1 - Föhlisch, Alexander A1 - Techert, Simone T1 - Probing the Hofmeister effect with ultrafast core-hole spectroscopy JF - The journal of physical chemistry : B, Condensed matter, materials, surfaces, interfaces & biophysical chemistry N2 - In the current work, X-ray emission spectra of aqueous solutions of different inorganic salts within the Hofmeister series are presented. The results reflect the direct interaction of the ions with the water molecules and therefore, reveal general properties of the salt-water interactions. Within the experimental precision a significant effect of the ions on the water structure has been observed but no ordering according to the structure maker/structure breaker concept could be mirrored in the results indicating that the Hofmeister effect if existent may be caused by more complex interactions. Y1 - 2014 U6 - https://doi.org/10.1021/jp504577a SN - 1520-6106 VL - 118 IS - 31 SP - 9398 EP - 9403 PB - American Chemical Society CY - Washington ER - TY - JOUR A1 - Levermann, Anders A1 - Winkelmann, Ricarda A1 - Nowicki, S. A1 - Fastook, J. L. A1 - Frieler, Katja A1 - Greve, R. A1 - Hellmer, H. H. A1 - Martin, M. A. A1 - Meinshausen, Malte A1 - Mengel, Matthias A1 - Payne, A. J. A1 - Pollard, D. A1 - Sato, T. A1 - Timmermann, R. A1 - Wang, Wei Li A1 - Bindschadler, Robert A. T1 - Projecting antarctic ice discharge using response functions from SeaRISE ice-sheet models JF - Earth system dynamics N2 - The largest uncertainty in projections of future sea-level change results from the potentially changing dynamical ice discharge from Antarctica. Basal ice-shelf melting induced by a warming ocean has been identified as a major cause for additional ice flow across the grounding line. Here we attempt to estimate the uncertainty range of future ice discharge from Antarctica by combining uncertainty in the climatic forcing, the oceanic response and the ice-sheet model response. The uncertainty in the global mean temperature increase is obtained from historically constrained emulations with the MAGICC-6.0 (Model for the Assessment of Greenhouse gas Induced Climate Change) model. The oceanic forcing is derived from scaling of the subsurface with the atmospheric warming from 19 comprehensive climate models of the Coupled Model Intercomparison Project (CMIP-5) and two ocean models from the EU-project Ice2Sea. The dynamic ice-sheet response is derived from linear response functions for basal ice-shelf melting for four different Antarctic drainage regions using experiments from the Sea-level Response to Ice Sheet Evolution (SeaRISE) intercomparison project with five different Antarctic ice-sheet models. The resulting uncertainty range for the historic Antarctic contribution to global sea-level rise from 1992 to 2011 agrees with the observed contribution for this period if we use the three ice-sheet models with an explicit representation of ice-shelf dynamics and account for the time-delayed warming of the oceanic subsurface compared to the surface air temperature. The median of the additional ice loss for the 21st century is computed to 0.07 m (66% range: 0.02-0.14 m; 90% range: 0.0-0.23 m) of global sea-level equivalent for the low-emission RCP-2.6 (Representative Concentration Pathway) scenario and 0.09 m (66% range: 0.04-0.21 m; 90% range: 0.01-0.37 m) for the strongest RCP-8.5. Assuming no time delay between the atmospheric warming and the oceanic subsurface, these values increase to 0.09 m (66% range: 0.04-0.17 m; 90% range: 0.02-0.25 m) for RCP-2.6 and 0.15 m (66% range: 0.07-0.28 m; 90% range: 0.04-0.43 m) for RCP-8.5. All probability distributions are highly skewed towards high values. The applied ice-sheet models are coarse resolution with limitations in the representation of grounding-line motion. Within the constraints of the applied methods, the uncertainty induced from different ice-sheet models is smaller than that induced by the external forcing to the ice sheets. Y1 - 2014 U6 - https://doi.org/10.5194/esd-5-271-2014 SN - 2190-4979 SN - 2190-4987 VL - 5 IS - 2 SP - 271 EP - 293 PB - Copernicus CY - Göttingen ER - TY - JOUR A1 - Albrecht, Steve A1 - Tumbleston, John R. A1 - Janietz, Silvia A1 - Dumsch, Ines A1 - Allard, Sybille A1 - Scherf, Ullrich A1 - Ade, Harald W. A1 - Neher, Dieter T1 - Quantifying charge extraction in organic solar cells: The case of fluorinated PCPDTBT JF - The journal of physical chemistry letters N2 - We introduce a new and simple method to quantify the effective extraction mobility in organic solar cells at low electric fields and charge carrier densities comparable to operation conditions under one sun illumination. By comparing steady-state carrier densities at constant illumination intensity and under open-circuit conditions, the gradient of the quasi-Fermi potential driving the current is estimated as a function of external bias and charge density. These properties are then related to the respective steady-state current to determine the effective extraction mobility. The new technique is applied to different derivatives of the well-known low-band-gap polymer PCPDTBT blended with PC70BM. We show that the slower average extraction due to lower mobility accounts for the moderate fill factor when solar cells are fabricated with mono- or difluorinated PCPDTBT. This lower extraction competes with improved generation and reduced nongeminate recombination, rendering the monofluorinated derivative the most efficient donor polymer. Y1 - 2014 U6 - https://doi.org/10.1021/jz500457b SN - 1948-7185 VL - 5 IS - 7 SP - 1131 EP - 1138 PB - American Chemical Society CY - Washington ER - TY - JOUR A1 - Makarava, Natallia A1 - Menz, Stephan A1 - Theves, Matthias A1 - Huisinga, Wilhelm A1 - Beta, Carsten A1 - Holschneider, Matthias T1 - Quantifying the degree of persistence in random amoeboid motion based on the Hurst exponent of fractional Brownian motion JF - Physical review : E, Statistical, nonlinear and soft matter physics N2 - Amoebae explore their environment in a random way, unless external cues like, e. g., nutrients, bias their motion. Even in the absence of cues, however, experimental cell tracks show some degree of persistence. In this paper, we analyzed individual cell tracks in the framework of a linear mixed effects model, where each track is modeled by a fractional Brownian motion, i.e., a Gaussian process exhibiting a long-term correlation structure superposed on a linear trend. The degree of persistence was quantified by the Hurst exponent of fractional Brownian motion. Our analysis of experimental cell tracks of the amoeba Dictyostelium discoideum showed a persistent movement for the majority of tracks. Employing a sliding window approach, we estimated the variations of the Hurst exponent over time, which allowed us to identify points in time, where the correlation structure was distorted ("outliers"). Coarse graining of track data via down-sampling allowed us to identify the dependence of persistence on the spatial scale. While one would expect the (mode of the) Hurst exponent to be constant on different temporal scales due to the self-similarity property of fractional Brownian motion, we observed a trend towards stronger persistence for the down-sampled cell tracks indicating stronger persistence on larger time scales. Y1 - 2014 U6 - https://doi.org/10.1103/PhysRevE.90.042703 SN - 1539-3755 SN - 1550-2376 VL - 90 IS - 4 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Emelianova, Yulia P. A1 - Kuznetsov, A. P. A1 - Turukina, Ludmila V. T1 - Quasi-periodic bifurcations and "amplitude death" in low-dimensional ensemble of van der Pol oscillators JF - Modern physics letters : A, Particles and fields, gravitation, cosmology, nuclear physics N2 - The dynamics of the four dissipatively coupled van der Pol oscillators is considered. Lyapunov chart is presented in the parameter plane. Its arrangement is discussed. We discuss the bifurcations of tori in the system at large frequency detuning of the oscillators. Here are quasi-periodic saddle-node, Hopf and Neimark-Sacker bifurcations. The effect of increase of the threshold for the "amplitude death" regime and the possibilities of complete and partial broadband synchronization are revealed. KW - Chain of van der Pol oscillators KW - Bifurcations of tori KW - Amplitude death KW - Broadband synchronization Y1 - 2014 U6 - https://doi.org/10.1016/j.physleta.2013.10.049 SN - 0375-9601 SN - 1873-2429 VL - 378 IS - 3 SP - 153 EP - 157 PB - Elsevier CY - Amsterdam ER - TY - JOUR A1 - Gao, Guan-Nan A1 - Wang, Min A1 - Lin, Jun A1 - Wu, Ning A1 - Tan, Cheng-Ming A1 - Kliem, Bernhard A1 - Su, Yang T1 - Radio observations of the fine structure inside a post-CME current sheet JF - Research in astronomy and astrophysics : a publication of the Chinese Astronomical Society and National Astronomical Observatories, Chinese Academy of Sciences N2 - A solar radio burst was observed in a coronal mass ejection/flare event by the Solar Broadband Radio Spectrometer at the Huairou Solar Observing Station on 2004 December 1. The data exhibited various patterns of plasma motions, suggestive of the interaction between sunward moving plasmoids and the flare loop system during the impulsive phase of the event. In addition to the radio data, the associated white-light, H alpha, extreme ultraviolet light, and soft and hard X-rays were also studied. KW - Sun: coronal mass ejections (CMEs) KW - Sun: flares KW - Sun: solar radio bursts KW - Sun: magnetic reconnection Y1 - 2014 U6 - https://doi.org/10.1088/1674-4527/14/7/006 SN - 1674-4527 VL - 14 IS - 7 SP - 843 EP - 854 PB - Chinese Astronomical Society and National Astronomical Observatories, Chinese Academy of Sciences CY - Beijing ER - TY - JOUR A1 - Schmaelzlin, Elmar A1 - Moralejo, Benito A1 - Rutowska, Monika A1 - Monreal-Ibero, Ana A1 - Sandin, Christer A1 - Tarcea, Nicolae A1 - Popp, Juergen A1 - Roth, Martin M. T1 - Raman imaging with a fiber-coupled multichannel spectrograph JF - Sensors N2 - Until now, spatially resolved Raman Spectroscopy has required to scan a sample under investigation in a time-consuming step-by-step procedure. Here, we present a technique that allows the capture of an entire Raman image with only one single exposure. The Raman scattering arising from the sample was collected with a fiber-coupled high-performance astronomy spectrograph. The probe head consisting of an array of 20 x 20 multimode fibers was linked to the camera port of a microscope. To demonstrate the high potential of this new concept, Raman images of reference samples were recorded. Entire chemical maps were received without the need for a scanning procedure. KW - multichannel Raman spectroscopy KW - astronomy spectrograph KW - optical fiber bundle KW - Raman imaging Y1 - 2014 U6 - https://doi.org/10.3390/s141121968 SN - 1424-8220 VL - 14 IS - 11 SP - 21968 EP - 21980 PB - MDPI CY - Basel ER - TY - JOUR A1 - Schreck, Simon A1 - Beye, Martin A1 - Sellberg, Jonas A. A1 - McQueen, Trevor A1 - Laksmono, Hartawan A1 - Kennedy, Brian A1 - Eckert, Sebastian A1 - Schlesinger, Daniel A1 - Nordlund, Dennis A1 - Ogasawara, Hirohito A1 - Sierra, Raymond G. A1 - Segtnan, Vegard H. A1 - Kubicek, Katharina A1 - Schlotter, William F. A1 - Dakovski, Georgi L. A1 - Moeller, Stefan P. A1 - Bergmann, Uwe A1 - Techert, Simone A1 - Pettersson, Lars G. M. A1 - Wernet, Philippe A1 - Bogan, Michael J. A1 - Harada, Yoshihisa A1 - Nilsson, Anders A1 - Föhlisch, Alexander T1 - Reabsorption of soft x-ray emission at high x-ray free-electron laserfluences JF - Physical review letters N2 - We report on oxygen K-edge soft x-ray emission spectroscopy from a liquid water jet at the Linac Coherent Light Source. We observe significant changes in the spectral content when tuning over a wide range of incident x-ray fluences. In addition the total emission yield decreases at high fluences. These modifications result from reabsorption of x-ray emission by valence-excited molecules generated by the Auger cascade. Our observations have major implications for future x-ray emission studies at intense x-ray sources. We highlight the importance of the x-ray pulse length with respect to the core-hole lifetime. Y1 - 2014 U6 - https://doi.org/10.1103/PhysRevLett.113.153002 SN - 0031-9007 SN - 1079-7114 VL - 113 IS - 15 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Tu, Rui A1 - Wang, Li T1 - Real-time coseismic wave retrieving by integrated Kalman filter with observations of GPS, Glonass and strong-motion sensor JF - Advances in space research N2 - A method of real-time coseismic wave retrieving was proposed based on the tight integration of GPS, Glonass and strong-motion sensor observations, the validation and precision analysis have been made by an experimental data. The series of results have been shown that: by the integrated Kalman filter and multi-sensors, the coseismic waves can be optimally recovered by complement the advantages of each other, especially when the observation conditions are very bad. In additional, the results are not significantly effected by different receiver clock error processes for the integration solution. KW - GPS and Glonass KW - Strong-motion sensor KW - Baseline shift KW - Integrated Kalman filter KW - Real-time earthquake monitoring and early warning Y1 - 2014 U6 - https://doi.org/10.1016/j.asr.2013.10.011 SN - 0273-1177 SN - 1879-1948 VL - 53 IS - 1 SP - 130 EP - 137 PB - Elsevier CY - Oxford ER - TY - JOUR A1 - Kralemann, Bjoern A1 - Pikovskij, Arkadij A1 - Rosenblum, Michael T1 - Reconstructing connectivity of oscillator networks from multimodal observations JF - Biomedizinische Technik = Biomedical engineering Y1 - 2014 U6 - https://doi.org/10.1515/bmt-2014-4089 SN - 0013-5585 SN - 1862-278X VL - 59 SP - S220 EP - S220 PB - De Gruyter CY - Berlin ER - TY - JOUR A1 - Kralemann, Bjoern A1 - Pikovskij, Arkadij A1 - Rosenblum, Michael T1 - Reconstructing effective phase connectivity of oscillator networks from observations JF - New journal of physics : the open-access journal for physics N2 - We present a novel approach for recovery of the directional connectivity of a small oscillator network by means of the phase dynamics reconstruction from multivariate time series data. The main idea is to use a triplet analysis instead of the traditional pairwise one. Our technique reveals an effective phase connectivity which is generally not equivalent to a structural one. We demonstrate that by comparing the coupling functions from all possible triplets of oscillators, we are able to achieve in the reconstruction a good separation between existing and non-existing connections, and thus reliably reproduce the network structure. KW - network reconstruction KW - coupled oscillators KW - connectivity KW - data analysis Y1 - 2014 U6 - https://doi.org/10.1088/1367-2630/16/8/085013 SN - 1367-2630 VL - 16 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Beshnova, Daria A. A1 - Cherstvy, Andrey G. A1 - Vainshtein, Yevhen A1 - Teif, Vladimir B. T1 - Regulation of the nucleosome repeat length in vivo by the DNA sequence, protein concentrations and long-range interactions JF - PLoS Computational Biology : a new community journal N2 - The nucleosome repeat length (NRL) is an integral chromatin property important for its biological functions. Recent experiments revealed several conflicting trends of the NRL dependence on the concentrations of histones and other architectural chromatin proteins, both in vitro and in vivo, but a systematic theoretical description of NRL as a function of DNA sequence and epigenetic determinants is currently lacking. To address this problem, we have performed an integrative biophysical and bioinformatics analysis in species ranging from yeast to frog to mouse where NRL was studied as a function of various parameters. We show that in simple eukaryotes such as yeast, a lower limit for the NRL value exists, determined by internucleosome interactions and remodeler action. For higher eukaryotes, also the upper limit exists since NRL is an increasing but saturating function of the linker histone concentration. Counterintuitively, smaller H1 variants or non-histone architectural proteins can initiate larger effects on the NRL due to entropic reasons. Furthermore, we demonstrate that different regimes of the NRL dependence on histone concentrations exist depending on whether DNA sequence-specific effects dominate over boundary effects or vice versa. We consider several classes of genomic regions with apparently different regimes of the NRL variation. As one extreme, our analysis reveals that the period of oscillations of the nucleosome density around bound RNA polymerase coincides with the period of oscillations of positioning sites of the corresponding DNA sequence. At another extreme, we show that although mouse major satellite repeats intrinsically encode well-defined nucleosome preferences, they have no unique nucleosome arrangement and can undergo a switch between two distinct types of nucleosome positioning. Y1 - 2014 U6 - https://doi.org/10.1371/journal.pcbi.1003698 SN - 1553-734X SN - 1553-7358 VL - 10 IS - 7 PB - PLoS CY - San Fransisco ER - TY - JOUR A1 - Baushev, Anton N. T1 - Relaxation of dark matter halos: how to match observational data? JF - Astronomy and astrophysics : an international weekly journal N2 - We show that moderate energy relaxation in the formation of dark matter halos invariably leads to profiles that match those observed in the central regions of galaxies. The density profile of the central region is universal and insensitive to either the seed perturbation shape or the details of the relaxation process. The profile has a central core; the multiplication of the central density by the core radius is almost independent of the halo mass, in accordance with observations. In the core area the density distribution behaves as an Einasto profile with low index (n similar to 0.5); it has an extensive region with rho proportional to r(-2) at larger distances. This is exactly the shape that observations suggest for the central region of galaxies. On the other hand, this shape does not fit the galaxy cluster profiles. A possible explanation of this fact is that the relaxation is violent in the case of galaxy clusters; however, it is not violent enough when galaxies or smaller dark matter structures are considered. We discuss the reasons for this. KW - dark matter KW - Galaxy: structure KW - Galaxy: formation KW - astroparticle physics KW - methods: analytical Y1 - 2014 U6 - https://doi.org/10.1051/0004-6361/201322730 SN - 0004-6361 SN - 1432-0746 VL - 569 PB - EDP Sciences CY - Les Ulis ER - TY - INPR A1 - Henkel, Carsten A1 - Pieplow, Gregor T1 - Reply to Comment on 'Fully covariant radiation force on a polarizable particle' T2 - New journal of physics : the open-access journal for physics N2 - We argue that the theories of Volokitin and Persson (2014 New J. Phys. 16 118001), Dedkov and Kyasov (2008 J. Phys.: Condens. Matter 20 354006), and Pieplow and Henkel (2013 New J. Phys. 15 023027) agree on the electromagnetic force on a small, polarizable particle that is moving parallel to a planar, macroscopic body, as far as the contribution of evanescent waves is concerned. The apparent differences are discussed in detail and explained by choices of units and integral transformations. We point out in particular the role of the Lorentz contraction in the procedure used by Volokitin and Persson, where a macroscopic body is 'diluted' to obtain the force on a small particle. Differences that appear in the contribution of propagating photons are briefly mentioned. KW - applied classical electromagnetism KW - fluctuation phenomena KW - random processes KW - noise KW - Brownian motion KW - mechanical effects of light Y1 - 2014 U6 - https://doi.org/10.1088/1367-2630/16/11/118002 SN - 1367-2630 VL - 16 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Jeon, Jae-Hyung A1 - Chechkin, Aleksei V. A1 - Metzler, Ralf T1 - Scaled Brownian motion: a paradoxical process with a time dependent diffusivity for the description of anomalous diffusion JF - Physical chemistry, chemical physics : PCCP N2 - Anomalous diffusion is frequently described by scaled Brownian motion (SBM){,} a Gaussian process with a power-law time dependent diffusion coefficient. Its mean squared displacement is ?x2(t)? [similar{,} equals] 2K(t)t with K(t) [similar{,} equals] t[small alpha]-1 for 0 < [small alpha] < 2. SBM may provide a seemingly adequate description in the case of unbounded diffusion{,} for which its probability density function coincides with that of fractional Brownian motion. Here we show that free SBM is weakly non-ergodic but does not exhibit a significant amplitude scatter of the time averaged mean squared displacement. More severely{,} we demonstrate that under confinement{,} the dynamics encoded by SBM is fundamentally different from both fractional Brownian motion and continuous time random walks. SBM is highly non-stationary and cannot provide a physical description for particles in a thermalised stationary system. Our findings have direct impact on the modelling of single particle tracking experiments{,} in particular{,} under confinement inside cellular compartments or when optical tweezers tracking methods are used. KW - single-particle tracking KW - living cells KW - random-walks KW - subdiffusion KW - dynamics KW - nonergodicity KW - coefficients KW - transport KW - membrane KW - behavior Y1 - 2014 U6 - https://doi.org/10.1039/C4CP02019G VL - 30 IS - 16 SP - 15811 EP - 15817 PB - The Royal Society of Chemistry CY - Cambridge ER - TY - GEN A1 - Jeon, Jae-Hyung A1 - Chechkin, Aleksei V. A1 - Metzler, Ralf T1 - Scaled Brownian motion: a paradoxical process with a time dependent diffusivity for the description of anomalous diffusion N2 - Anomalous diffusion is frequently described by scaled Brownian motion (SBM){,} a Gaussian process with a power-law time dependent diffusion coefficient. Its mean squared displacement is ?x2(t)? [similar{,} equals] 2K(t)t with K(t) [similar{,} equals] t[small alpha]-1 for 0 < [small alpha] < 2. SBM may provide a seemingly adequate description in the case of unbounded diffusion{,} for which its probability density function coincides with that of fractional Brownian motion. Here we show that free SBM is weakly non-ergodic but does not exhibit a significant amplitude scatter of the time averaged mean squared displacement. More severely{,} we demonstrate that under confinement{,} the dynamics encoded by SBM is fundamentally different from both fractional Brownian motion and continuous time random walks. SBM is highly non-stationary and cannot provide a physical description for particles in a thermalised stationary system. Our findings have direct impact on the modelling of single particle tracking experiments{,} in particular{,} under confinement inside cellular compartments or when optical tweezers tracking methods are used. T3 - Zweitveröffentlichungen der Universität Potsdam : Mathematisch-Naturwissenschaftliche Reihe - 180 KW - single-particle tracking KW - living cells KW - random-walks KW - subdiffusion KW - dynamics KW - nonergodicity KW - coefficients KW - transport KW - membrane KW - behavior Y1 - 2014 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-76302 SP - 15811 EP - 15817 ER - TY - JOUR A1 - Mulansky, Mario T1 - Scaling of chaos in strongly nonlinear lattices JF - Chaos : an interdisciplinary journal of nonlinear science N2 - Although it is now understood that chaos in complex classical systems is the foundation of thermodynamic behavior, the detailed relations between the microscopic properties of the chaotic dynamics and the macroscopic thermodynamic observations still remain mostly in the dark. In this work, we numerically analyze the probability of chaos in strongly nonlinear Hamiltonian systems and find different scaling properties depending on the nonlinear structure of the model. We argue that these different scaling laws of chaos have definite consequences for the macroscopic diffusive behavior, as chaos is the microscopic mechanism of diffusion. This is compared with previous results on chaotic diffusion [M. Mulansky and A. Pikovsky, New J. Phys. 15, 053015 (2013)], and a relation between microscopic chaos and macroscopic diffusion is established. (C) 2014 AIP Publishing LLC. Y1 - 2014 U6 - https://doi.org/10.1063/1.4868259 SN - 1054-1500 SN - 1089-7682 VL - 24 IS - 2 PB - American Institute of Physics CY - Melville ER - TY - JOUR A1 - Tobie, G. A1 - Teanby, N. A. A1 - Coustenis, A. A1 - Jaumann, Ralf A1 - Raulin, E. A1 - Schmidt, J. A1 - Carrasco, N. A1 - Coates, Andrew J. A1 - Cordier, D. A1 - De Kok, R. A1 - Geppert, W. D. A1 - Lebreton, J. -P. A1 - Lefevre, A. A1 - Livengood, T. A. A1 - Mandt, K. E. A1 - Mitri, G. A1 - Nimmo, F. A1 - Nixon, C. A. A1 - Norman, L. A1 - Pappalardo, R. T. A1 - Postberg, F. A1 - Rodriguez, S. A1 - SchuizeMakuch, D. A1 - Soderblom, J. M. A1 - Solomonidou, A. A1 - Stephan, K. A1 - Stofan, E. R. A1 - Turtle, E. P. A1 - Wagner, R. J. A1 - West, R. A. A1 - Westlake, J. H. T1 - Science goals and mission concept for the future exploration of Titan and Enceladus JF - Planetary and space science KW - Titan KW - Enceladus KW - Atmosphere KW - Surface KW - Ocean KW - Interior KW - Missions Y1 - 2014 U6 - https://doi.org/10.1016/j.pss.2014.10.002 SN - 0032-0633 VL - 104 SP - 59 EP - 77 PB - Elsevier CY - Oxford ER - TY - JOUR A1 - Sborikas, Martynas A1 - Qiu, Xunlin A1 - Wirges, Werner A1 - Gerhard, Reimund A1 - Jenninger, Werner A1 - Lovera, Deliani T1 - Screen printing for producing ferroelectret systems with polymer-electret films and well-defined cavities JF - Applied physics : A, Materials science & processing N2 - We report a process for preparing polymer ferroelectrets by means of screen printing-a technology that is widely used for the two-dimensional patterning of printed layers. In order to produce polymer-film systems with cavities that are suitable for bipolar electric charging, a screen-printing paste is deposited through a screen with a pre-designed pattern onto the surface of a polymer electret film. Another such polymer film is placed on top of the printed pattern, and well-defined cavities are formed in-between. During heating and curing, the polymer films are tightly bonded to the patterned paste layer so that a stable three-layer system is obtained. In the present work, polycarbonate (PC) films have been employed as electret layers. Screen printing, curing and charging led to PC ferroelectret systems with a piezoelectric d (33) coefficient of about 28 pC/N that is stable up to 100 C-a similar to. Due to the rather soft patterned layer, d (33) strongly decreases already for static pressures of tens of kPa. The results demonstrate the suitability of screen printing for the preparation of ferroelectret systems. Y1 - 2014 U6 - https://doi.org/10.1007/s00339-013-7998-3 SN - 0947-8396 SN - 1432-0630 VL - 114 IS - 2 SP - 515 EP - 520 PB - Springer CY - New York ER - TY - JOUR A1 - Abramowski, Attila A1 - Aharonian, Felix A. A1 - Benkhali, Faical Ait A1 - Akhperjanian, A. G. A1 - Angüner, Ekrem Oǧuzhan A1 - Backes, Michael A1 - Balenderan, Shangkari A1 - Balzer, Arnim A1 - Barnacka, Anna A1 - Becherini, Yvonne A1 - Tjus, J. Becker A1 - Berge, David A1 - Bernhard, Sabrina A1 - Bernlöhr, K. A1 - Birsin, E. A1 - Biteau, Jonathan A1 - Boettcher, Markus A1 - Boisson, Catherine A1 - Bolmont, J. A1 - Bordas, Pol A1 - Bregeon, Johan A1 - Brun, Francois A1 - Brun, Pierre A1 - Bryan, Mark A1 - Bulik, Tomasz A1 - Carrigan, Svenja A1 - Casanova, Sabrina A1 - Chadwick, Paula M. A1 - Chakraborty, N. A1 - Chalme-Calvet, R. A1 - Chaves, Ryan C. G. A1 - Chretien, M. A1 - Colafrancesco, Sergio A1 - Cologna, Gabriele A1 - Conrad, Jan A1 - Couturier, C. A1 - Cui, Y. A1 - Dalton, M. A1 - Davids, I. D. A1 - Degrange, B. A1 - Deil, C. A1 - deWilt, P. A1 - Djannati-Ataï, A. A1 - Domainko, W. A1 - Donath, A. A1 - Dubus, G. A1 - Dutson, K. A1 - Dyks, J. A1 - Dyrda, M. A1 - Edwards, T. A1 - Egberts, Kathrin A1 - Eger, P. A1 - Espigat, P. A1 - Farnier, C. A1 - Fegan, S. A1 - Feinstein, F. A1 - Fernandes, M. V. A1 - Fernandez, D. A1 - Fiasson, A. A1 - Fontaine, G. A1 - Foerster, A. A1 - Fuessling, M. A1 - Gabici, S. A1 - Gajdus, M. A1 - Gallant, Y. A. A1 - Garrigoux, T. A1 - Giavitto, G. A1 - Giebels, B. A1 - Glicenstein, J. F. A1 - Gottschall, D. A1 - Goudelis, A. A1 - Grondin, M. -H. A1 - Grudzinska, M. A1 - Hadsch, D. A1 - Haeffner, S. A1 - Hahn, J. A1 - Harris, J. A1 - Heinzelmann, G. A1 - Henri, G. A1 - Hermann, G. A1 - Hervet, O. A1 - Hillert, A. A1 - Hinton, James Anthony A1 - Hofmann, W. A1 - Hofverberg, P. A1 - Holler, M. A1 - Horns, D. A1 - Ivascenko, A. A1 - Jacholkowska, A. A1 - Jahn, C. A1 - Jamrozy, M. A1 - Janiak, M. A1 - Jankowsky, F. A1 - Jung, I. A1 - Kastendieck, M. A. A1 - Katarzynski, K. A1 - Katz, U. A1 - Kaufmann, S. A1 - Khelifi, B. A1 - Kieffer, M. A1 - Klepser, S. A1 - Klochkov, D. A1 - Kluzniak, W. A1 - Kolitzus, D. A1 - Komin, Nu. A1 - Kosack, K. A1 - Krakau, S. A1 - Krayzel, F. A1 - Krueger, P. P. A1 - Laffon, H. A1 - Lamanna, G. A1 - Lefaucheur, J. A1 - Lefranc, V. A1 - Lemiere, A. A1 - Lemoine-Goumard, M. A1 - Lenain, J. -P. A1 - Lohse, T. A1 - Lopatin, A. A1 - Lu, C. -C. A1 - Marandon, V. A1 - Marcowith, Alexandre A1 - Marx, R. A1 - Maurin, G. A1 - Maxted, N. A1 - Mayer, M. A1 - McComb, T. J. L. A1 - Mehault, J. A1 - Meintjes, P. J. A1 - Menzler, U. A1 - Meyer, M. A1 - Mitchell, A. M. W. A1 - Moderski, R. A1 - Mohamed, M. A1 - Mora, K. A1 - Moulin, Emmanuel A1 - Murach, T. A1 - de Naurois, M. A1 - Niemiec, J. A1 - Nolan, S. J. A1 - Oakes, L. A1 - Odaka, H. A1 - Ohm, S. A1 - Opitz, B. A1 - Ostrowski, M. A1 - Oya, I. A1 - Panter, M. A1 - Parsons, R. D. A1 - Arribas, M. Paz A1 - Pekeur, N. W. A1 - Pelletier, G. A1 - Perez, J. A1 - Petrucci, P. -O. A1 - Peyaud, B. A1 - Pita, S. A1 - Poon, H. A1 - Puehlhofer, G. A1 - Punch, M. A1 - Quirrenbach, A. A1 - Raab, S. A1 - Reichardt, I. A1 - Reimer, A. A1 - Reimer, Olaf A1 - Renaud, M. A1 - de los Reyes, R. A1 - Rieger, F. A1 - Rob, L. A1 - Romoli, C. A1 - Rosier-Lees, S. A1 - Rowell, G. A1 - Rudak, B. A1 - Rulten, C. B. A1 - Sahakian, V. A1 - Salek, D. A1 - Sanchez, David M. A1 - Santangelo, Andrea A1 - Schlickeiser, R. A1 - Schuessler, Fabian A1 - Schulz, A. A1 - Schwanke, U. A1 - Schwarzburg, S. A1 - Schwemmer, S. A1 - Serpico, P. A1 - Sol, H. A1 - Spanier, F. A1 - Spengler, G. A1 - Spiess, F. A1 - Steenkamp, R. A1 - Stegmann, Christian A1 - Stinzing, F. A1 - Stycz, K. A1 - Sushch, Iurii A1 - Tavernet, J. -P. A1 - Tavernier, T. A1 - Taylor, A. M. A1 - Terrier, R. A1 - Tluczykont, M. A1 - Trichard, C. A1 - Valerius, K. A1 - van Eldik, C. A1 - van Soelen, B. A1 - Vasileiadis, G. A1 - Veh, J. A1 - Venter, C. A1 - Viana, A. A1 - Vincent, P. A1 - Vink, J. A1 - Voelk, H. J. A1 - Volpe, F. A1 - Vorster, M. A1 - Vuillaume, T. A1 - Wagner, S. J. A1 - Wagner, P. A1 - Wagner, R. M. A1 - Ward, M. A1 - Weidinger, M. A1 - Weitzel, Q. A1 - White, R. A1 - Wierzcholska, A. A1 - Willmann, P. A1 - Woernlein, A. A1 - Wouters, D. A1 - Yang, R. A1 - Zabalza, V. A1 - Zaborov, D. A1 - Zacharias, M. A1 - Zdziarski, A. A. A1 - Zech, Alraune A1 - Zechlin, H. -S. T1 - Search for dark matter annihilation signatures in HESS observations of dwarf spheroidal galaxies JF - Physical review : D, Particles, fields, gravitation, and cosmology N2 - Dwarf spheroidal galaxies of the Local Group are close satellites of the Milky Way characterized by a large mass-to-light ratio and are not expected to be the site of nonthermal high-energy gamma-ray emission or intense star formation. Therefore they are among the most promising candidates for indirect dark matter searches. During the last years the High Energy Stereoscopic System (H.E.S.S.) of imaging atmospheric Cherenkov telescopes observed five of these dwarf galaxies for more than 140 hours in total, searching for TeV gamma-ray emission from annihilation of dark matter particles. The new results of the deep exposure of the Sagittarius dwarf spheroidal galaxy, the first observations of the Coma Berenices and Fornax dwarves and the reanalysis of two more dwarf spheroidal galaxies already published by the H.E.S.S. Collaboration, Carina and Sculptor, are presented. In the absence of a significant signal new constraints on the annihilation cross section applicable to weakly interacting massive particles (WIMPs) are derived by combining the observations of the five dwarf galaxies. The combined exclusion limit depends on the WIMP mass and the best constraint is reached at 1-2 TeV masses with a cross-section upper bound of similar to 3.9 x 10(-24) cm(3) s(-1) at a 95% confidence level. Y1 - 2014 U6 - https://doi.org/10.1103/PhysRevD.90.112012 SN - 1550-7998 SN - 1550-2368 VL - 90 IS - 11 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Abramowski, Attila A1 - Aharonian, Felix A. A1 - Benkhali, Faical Ait A1 - Akhperjanian, A. G. A1 - Angüner, Ekrem Oǧuzhan A1 - Anton, Gisela A1 - Backes, Michael A1 - Balenderan, Shangkari A1 - Balzer, Arnim A1 - Barnacka, Anna A1 - Becherini, Yvonne A1 - Tjus, J. Becker A1 - Bernlöhr, K. A1 - Birsin, E. A1 - Bissaldi, E. A1 - Biteau, Jonathan A1 - Boettcher, Markus A1 - Boisson, Catherine A1 - Bolmont, J. A1 - Bordas, Pol A1 - Brucker, J. A1 - Brun, Francois A1 - Brun, Pierre A1 - Bulik, Tomasz A1 - Carrigan, Svenja A1 - Casanova, Sabrina A1 - Chadwick, Paula M. A1 - Chalme-Calvet, R. A1 - Chaves, Ryan C. G. A1 - Cheesebrough, A. A1 - Chretien, M. A1 - Colafrancesco, Sergio A1 - Cologna, Gabriele A1 - Conrad, Jan A1 - Couturier, C. A1 - Cui, Y. A1 - Djannati-Ataï, A. A1 - Domainko, W. A1 - Dubus, G. A1 - Dutson, K. A1 - Dyks, J. A1 - Dyrda, M. A1 - Edwards, T. A1 - Egberts, Kathrin A1 - Eger, P. A1 - Espigat, P. A1 - Farnier, C. A1 - Fegan, S. A1 - Feinstein, F. A1 - Fernandes, M. V. A1 - Fernandez, D. A1 - Fiasson, A. A1 - Fontaine, G. A1 - Foerster, A. A1 - Fussling, Matthias A1 - Gajdus, M. A1 - Gallant, Y. A. A1 - Garrigoux, T. A1 - Giavitto, G. A1 - Giebels, B. A1 - Glicenstein, J. F. A1 - Grondin, M. -H. A1 - Grudzinska, M. A1 - Haeffner, S. A1 - Hahn, J. A1 - Harris, J. A1 - Heinzelmann, G. A1 - Henri, G. A1 - Hermann, G. A1 - Hervet, O. A1 - Hillert, A. A1 - Hinton, James Anthony A1 - Hofmann, W. A1 - Hofverberg, P. A1 - Holler, M. A1 - Horns, D. A1 - Jacholkowska, A. A1 - Jahn, C. A1 - Jamrozy, M. A1 - Janiak, M. A1 - Jankowsky, F. A1 - Jung, I. A1 - Kastendieck, M. A. A1 - Katarzynski, K. A1 - Katz, U. A1 - Kaufmann, S. A1 - Khelifi, B. A1 - Kieffer, M. A1 - Klepser, S. A1 - Klochkov, D. A1 - Kluzniak, W. A1 - Kneiske, T. A1 - Kolitzus, D. A1 - Komin, Nu. A1 - Kosack, K. A1 - Krakau, S. A1 - Krayzel, F. A1 - Krueger, P. P. A1 - Laffon, H. A1 - Lamanna, G. A1 - Lefaucheur, J. A1 - Lemiere, A. A1 - Lemoine-Goumard, M. A1 - Lenain, J. -P. A1 - Lohse, T. A1 - Lopatin, A. A1 - Lu, C. -C. A1 - Marandon, V. A1 - Marcowith, Alexandre A1 - Marx, R. A1 - Maurin, G. A1 - Maxted, N. A1 - Mayer, M. A1 - McComb, T. J. L. A1 - Mehault, J. A1 - Meintjes, P. J. A1 - Menzler, U. A1 - Meyer, M. A1 - Moderski, R. A1 - Mohamed, M. A1 - Moulin, Emmanuel A1 - Murach, T. A1 - Naumann, C. L. A1 - de Naurois, M. A1 - Niemiec, J. A1 - Nolan, S. J. A1 - Oakes, L. A1 - Odaka, H. A1 - Ohm, S. A1 - Wilhelmi, E. de Ona A1 - Opitz, B. A1 - Ostrowski, M. A1 - Oya, I. A1 - Panter, M. A1 - Parsons, R. D. A1 - Arribas, M. Paz A1 - Pekeur, N. W. A1 - Pelletier, G. A1 - Perez, J. A1 - Petrucci, P. -O. A1 - Peyaud, B. A1 - Pita, S. A1 - Poon, H. A1 - Puehlhofer, G. A1 - Punch, M. A1 - Quirrenbach, A. A1 - Raab, S. A1 - Raue, M. A1 - Reichardt, I. A1 - Reimer, A. A1 - Reimer, O. A1 - Renaud, M. A1 - Reyes, R. de los A1 - Rieger, F. A1 - Rob, L. A1 - Romoli, C. A1 - Rosier-Lees, S. A1 - Rowell, G. A1 - Rudak, B. A1 - Rulten, C. B. A1 - Sahakian, V. A1 - Sanchez, David M. A1 - Santangelo, Andrea A1 - Schlickeiser, R. A1 - Schuessler, F. A1 - Schulz, A. A1 - Schwanke, U. A1 - Schwarzburg, S. A1 - Schwemmer, S. A1 - Sol, H. A1 - Spengler, G. A1 - Spies, F. A1 - Stawarz, L. A1 - Steenkamp, R. A1 - Stegmann, Christian A1 - Stinzing, F. A1 - Stycz, K. A1 - Sushch, Iurii A1 - Tavernet, J. -P. A1 - Tavernier, T. A1 - Taylor, A. M. A1 - Terrier, R. A1 - Tluczykont, M. A1 - Trichard, C. A1 - Valerius, K. A1 - van Eldik, C. A1 - van Soelen, B. A1 - Vasileiadis, G. A1 - Venter, C. A1 - Viana, A. A1 - Vincent, P. A1 - Voelk, H. J. A1 - Volpe, F. A1 - Vorster, M. A1 - Vuillaume, T. A1 - Wagner, S. J. A1 - Wagner, P. A1 - Wagner, R. M. A1 - Ward, M. A1 - Weidinger, M. A1 - Weitzel, Q. A1 - White, R. A1 - Wierzcholska, A. A1 - Willmann, P. A1 - Woernlein, A. A1 - Wouters, D. A1 - Yang, R. A1 - Zabalza, V. A1 - Zacharias, M. A1 - Zdziarski, A. A. A1 - Zech, Alraune A1 - Zechlin, H. -S. A1 - Malyshev, D. T1 - Search for extended gamma-ray emission around AGN with HESS and Fermi-LAT JF - Astronomy and astrophysics : an international weekly journal N2 - Context. Very-high-energy (VHE; E > 100 GeV) gamma-ray emission from blazars inevitably gives rise to electron-positron pair production through the interaction of these gamma-rays with the extragalactic background light (EBL). Depending on the magnetic fields in the proximity of the source, the cascade initiated from pair production can result in either an isotropic halo around an initially- beamed source or a magnetically- broadened cascade :aux. Aims. Both extended pair-halo (PH) and magnetically broadened cascade (MBC) emission from regions surrounding the blazars 1ES 1101-232, IRS 0229+200, and PKS 2155-304 were searched for using VHE y-ray data taken with the High Energy Stereoscopic System (HESS.) and high-energy (HE; 100 MeV < E < 100 GeV) gamma-ray data with the Fermi Large Area Telescope (LAT). Methods. By comparing the angular distributions of the reconstructed gamma-ray events to the angular profiles calculated from detailed theoretical models, the presence of PH and MBC was investigated. Results. Upper limits on the extended emission around lES 1101-232, lES 0229+200, and PKS 2155-304 are found to be at a level of a few per cent of the Crab nebula flux above 1 TeV, depending on the assumed photon index of the cascade emission. Assuming strong extra-Galactic magnetic field (EGME) values, >10(-12) G, this limits the production of pair haloes developing from electromagnetic cascades. For weaker magnetic fields, in which electromagnetic cascades would result in MBCs. EGMF strengths in the range (0.3-3) x 10(-15) G were excluded for PKS 2155-304 at the 99% confidence level, under the assumption of a 1 Mpc coherence length. KW - gamma rays: galaxies KW - galaxies: magnetic fields KW - intergalactic medium KW - BL Lacertae objects: individual: PKS 2155-304 KW - BL Lacertae objects: individual: lES 1101-232 KW - BL Lacertae objects: individual: lES 0229+200 Y1 - 2014 U6 - https://doi.org/10.1051/0004-6361/201322510 SN - 0004-6361 SN - 1432-0746 VL - 562 PB - EDP Sciences CY - Les Ulis ER - TY - THES A1 - Schulz, Anneli T1 - Search for gamma-ray emission from bow shocks of runaway stars T1 - Suche nach Gammastrahlungsemission aus Bugwellen von Schnellläufersternen N2 - The mystery of the origin of cosmic rays has been tackled for more than hundred years and is still not solved. Cosmic rays are detected with energies spanning more than 10 orders of magnitude and reaching energies up to ~10²¹ eV, far higher than any man-made accelerator can reach. Different theories on the astrophysical objects and processes creating such highly energetic particles have been proposed. A very prominent explanation for a process producing highly energetic particles is shock acceleration. The observation of high-energy gamma rays from supernova remnants, some of them revealing a shell like structure, is clear evidence that particles are accelerated to ultrarelativistic energies in the shocks of these objects. The environments of supernova remnants are complex and challenge detailed modelling of the processes leading to high-energy gamma-ray emission. The study of shock acceleration at bow shocks, created by the supersonic movement of individual stars through the interstellar medium, offers a unique possibility to determine the physical properties of shocks in a less complex environment. The shocked medium is heated by the stellar and the shock excited radiation, leading to thermal infrared emission. 28 bow shocks have been discovered through their infrared emission. Nonthermal radiation in radio and X-ray wavelengths has been detected from two bow shocks, pointing to the existence of relativistic particles in these systems. Theoretical models of the emission processes predict high-energy and very high-energy emission at a flux level in reach of current instruments. This work presents the search for gamma-ray emission from bow shocks of runaway stars in the energy regime from 100MeV to ~100TeV. The search is performed with the large area telescope (LAT) on-board the Fermi satellite and the H.E.S.S. telescopes located in the Khomas Highland in Namibia. The Fermi-LAT was launched in 2008 and is continuously scanning the sky since then. It detects photons with energies from 20MeV to over 300 GeV and has an unprecedented sensitivity. The all-sky coverage allows us to study all 28 bow shocks of runaway stars listed in the E-BOSS catalogue of infrared bow shocks. No significant emission was detected from any of the objects, although predicted by several theoretical models describing the non-thermal emission of bow shocks of runaway stars. The H.E.S.S. experiment is the most sensitive system of imaging atmospheric Cherenkov telescopes. It detects photons from several tens of GeV to ~100TeV. Seven of the bow shocks have been observed with H.E.S.S. and the data analysis is presented in this thesis. The analyses of the very-high energy data did not reveal significant emission from any of the sources either. This work presents the first systematic search for gamma-ray emission from bow shocks of runaway stars. For the first time Fermi-LAT data was specifically analysed to reveal emission from bow shocks of runaway stars. In the TeV regime no searches for emission from theses objects have been published so far, the study presented here is the first in this energy regime. The level of the gamma-ray emission from bow shocks of runaway stars is constrained by the calculated upper limits over six orders in magnitude in energy. The upper limits calculated for the bow shocks of runaway stars in the course of this work, constrain several models. For the best candidate, ζ Ophiuchi, the upper limits in the Fermi-LAT energy range are lower than the predictions by a factor ~5. This challenges the assumptions made in this model and gives valuable input for further modelling approaches. The analyses were performed with the software packages provided by the H.E.S.S. and Fermi collaborations. The development of a unified analysis framework for gamma-ray data, namely GammaLib/ctools, is rapidly progressing within the CTA consortium. Recent implementations and cross-checks with current software frameworks are presented in the Appendix. N2 - Das Rätsel des Ursprungs der kosmischen Strahlung wird seit über 100 Jahren angegangen und ist noch immer nicht gelöst. Kosmische Strahlung wird mit Energien die zehn Größenordnungen überspannen gemessen und erreicht Energien bis zu ~10²¹ eV, weit höher als irgendein menschengemachter Beschleuniger erzeugen kann. Verschiedene Theorien über die astrophysikalischen Objekte und Prozesse, die solch hochenergetische Teilchen erzeugen können, wurden vorgeschlagen. Eine prominente Erklärung für einen Prozess, der hochenergetische Teilchen erzeugt ist Schockbeschleunigung. Die Detektion von hochenergetischer Gammastrahlung von Supernovaüberresten, von denen einige schalenförmige Strukturen offenbarten, ist ein klarer Beweis für die Beschleunigung von Teilchen zu ultrarelativistischen Energien in den Schocks dieser Objekte. Die Umgebung von Supernovaüberresten ist komplex und das detaillierte Modellieren der Prozesse die zu hochenergetischer Gammastrahlung führen herausfordernd. Die Untersuchung von Schockbeschleunigung an Bugwellen, die durch individuelle Sterne erzeugt werden, die sich mit Überschallgeschwindigkeit durch das interstellare Medium bewegen, bietet die einmalige Gelegenheit die physikalischen Eigenschaften von Schocks in einer weniger komplexen Umgebung zu bestimmen. Das komprimierte ("geschockte") Medium wird durch die Strahlung des Sterns und die durch den Schock angeregte Strahlung erhitzt und sendet infolgedessen thermische Infrarot-Strahlung aus. Nichtthermische Strahlung, die auf die Existenz von relativistischen Teilchen hinweist, wurde von zwei Bugwellen in Radio- und Röntgen-Wellenlängen gemessen. Theoretische Modelle der Strahlungsprozesse sagen hochenergetische und sehr hochenergetische Strahlung auf einem Niveau, welches mit aktuellen Instrumenten gemessen werden kann, voraus. Diese Arbeit präsentiert die Suche nach hochenergetischer Gammastrahung von Bugwellen von Schnellläufersternen in einem Energiebereich von 100MeV bis ~100TeV. Diese Suche wird mit dem "large area telescope"(LAT) an Bord des Fermi Satelliten und den H.E.S.S. Teleskopen, die im Khomas Hochland in Namibia in Betrieb sind, durchgeführt. Der Fermi Satellit wurde 2008 gestartet und das Fermi-LAT durchmustert seitdem kontinuierlich den Himmel. Es detektiert Photonen im Energiebereich von 20MeV bis über 300GeV und hat eine noch nie dagewesene Sensitivität. Die Abdeckung des gesamten Himmels erlaubt es alle 28 Bugwellen von Schnellläufersternen, die im E-BOSS Katalog aufgelistet sind, zu untersuchen. Von keiner der Bugwellen der Schnellläufersterne konnte signifikante Strahlung nachgewiesen werden, obwohl diese von theoretischen Modellen, die die nichtthermische Emission von Bugwellen von Schnellläufersternen beschreiben, vorausgesagt wurde. Das H.E.S.S. Experiment ist das sensitivste System von abbildenden Cherenkovteleskopen. Es kann Photonen mit Energien von einigen zehn GeV bis zu ~100TeV nachweisen. Sieben der Bugwellen von Schnellläufersternen wurden mit H.E.S.S. beobachtet und die Analyse der Daten wird in dieser Arbeit präsentiert. Auch die Analysen der sehr hochenergetischen Strahlung enthüllten keine signifikante Strahlung aus den Bugwellen der Schnellläufersterne. Diese Arbeit stellt die erste systematische Suche nach Gammastrahlung aus Bugwellen von Schnellläufersternen vor. Zum ersten Mal wurden Fermi-LAT Daten speziell zur Suche nach Emission von diesen Objekten analysiert. Im TeV-Energiebereich wurden bisher noch keine Suchen nach Gammastrahlung von Schnellläufersternen publiziert, die hier vorgestellte Studie ist also die erste in diesem Energiebereich. Das Niveau des Gammastrahlungflusses von Schnellläufersternen wird über einen sechs Größenordnungen überspannenden Energiebereich eingeschränkt. Die oberen Grenzen des Gammastrahlungs usses aus Bugwellen von Schnellläufersternen schränken verschiedene Modelle ein. Für den besten Kandidaten, ζ Ophiuchi, liegen die berechneten oberen Grenzen im Fermi-LAT Energiebereich einen Faktor ~5 unter den Vorhersagen. Dies fordert die Annahmen des Modells heraus und liefert wertvolle Bedingungen für weitere Modellierungsansätze. Die präsentierten Analysen wurden mit den Softwarepakten, die von den Fermi und H.E.S.S. Kollaborationen zur Verfügung gestellt werden, durchgeführt. Die Entwicklung einer gemeinsamen Analyseumgebung namens GammaLib/ctools wird im Rahmen des CTA Konsortiums umgesetzt. Neue Implementierungen und Gegenproben zu den momentanen Analyseumgebungen werden im Anhang präsentiert. KW - Gammastrahlungsastronomie KW - Fermi-LAT KW - H.E.S.S. KW - GammaLib/ctools KW - Bugwellenschocks KW - Schnellläufersterne KW - gamma-ray astronomy KW - Fermi KW - H.E.S.S KW - gammalib/ctools KW - bow shocks KW - runaway stars Y1 - 2014 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-73905 ER - TY - JOUR A1 - Abramowski, Attila A1 - Aharonian, Felix A. A1 - Benkhali, Faical Ait A1 - Akhperjanian, A. G. A1 - Angüner, Ekrem Oǧuzhan A1 - Anton, Gisela A1 - Balenderan, Shangkari A1 - Balzer, Arnim A1 - Barnacka, Anna A1 - Becherini, Yvonne A1 - Tjus, J. Becker A1 - Bernlöhr, K. A1 - Birsin, E. A1 - Bissaldi, E. A1 - Biteau, Jonathan A1 - Boettcher, Markus A1 - Boisson, Catherine A1 - Bolmont, J. A1 - Bordas, Pol A1 - Brucker, J. A1 - Brun, Francois A1 - Brun, Pierre A1 - Bulik, Tomasz A1 - Carrigan, Svenja A1 - Casanova, Sabrina A1 - Cerruti, M. A1 - Chadwick, Paula M. A1 - Chalme-Calvet, R. A1 - Chaves, Ryan C. G. A1 - Cheesebrough, A. A1 - Chretien, M. A1 - Colafrancesco, Sergio A1 - Cologna, Gabriele A1 - Conrad, Jan A1 - Couturier, C. A1 - Dalton, M. A1 - Daniel, M. K. A1 - Davids, I. D. A1 - Degrange, B. A1 - Deil, C. A1 - deWilt, P. A1 - Dicldnson, H. J. A1 - Djannati-Ataï, A. A1 - Domainko, W. A1 - Dubus, G. A1 - Dutson, K. A1 - Dyks, J. A1 - Dyrda, M. A1 - Edwards, T. A1 - Egberts, Kathrin A1 - Eger, P. A1 - Espigat, P. A1 - Farnier, C. A1 - Fegan, S. A1 - Feinstein, F. A1 - Fernandes, M. V. A1 - Fernandez, D. A1 - Fiasson, A. A1 - Fontaine, G. A1 - Foerster, A. A1 - Fuessling, Matthias A1 - Gajdus, M. A1 - Gallant, Y. A. A1 - Garrigoux, T. A1 - Giebels, B. A1 - Glicenstein, J. F. A1 - Grondin, M-H A1 - Grudzinska, M. A1 - Haeffner, S. A1 - Hahn, J. A1 - Harris, J. A1 - Heinzelmann, G. A1 - Henri, G. A1 - Hermann, G. A1 - Hervet, O. A1 - Hillert, A. A1 - Hinton, James Anthony A1 - Hofmann, W. A1 - Hofverberg, P. A1 - Holler, Markus A1 - Horns, D. A1 - Jacholkowska, A. A1 - Jahn, C. A1 - Jamrozy, M. A1 - Janiak, M. A1 - Jankowsky, F. A1 - Jung, I. A1 - Kastendieck, M. A. A1 - Katarzynski, K. A1 - Katz, U. A1 - Kaufmann, S. A1 - Khelifi, B. A1 - Kieffer, M. A1 - Klepser, S. A1 - Klochkov, D. A1 - Kluzniak, W. A1 - Kneiske, T. A1 - Kolitzus, D. A1 - Komin, Nu A1 - Kosack, K. A1 - Krakau, S. A1 - Krayzel, F. A1 - Krueger, P. P. A1 - Laffon, H. A1 - Lamanna, G. A1 - Lefaucheur, J. A1 - Lemiere, A. A1 - Lemoine-Goumard, M. A1 - Lenain, J-P A1 - Lennarz, D. A1 - Lohse, T. A1 - Lopatin, A. A1 - Lu, C-C A1 - Marandon, V. A1 - Marcowith, Alexandre A1 - Marx, R. A1 - Maurin, G. A1 - Maxted, N. A1 - Mayer, M. A1 - McComb, T. J. L. A1 - Mehault, J. A1 - Menzler, U. A1 - Meyer, M. A1 - Moderski, R. A1 - Mohamed, M. A1 - Moulin, Emmanuel A1 - Murach, T. A1 - Naumann, C. L. A1 - de Naurois, M. A1 - Niemiec, J. A1 - Nolan, S. J. A1 - Oakes, L. A1 - Ohm, S. A1 - Wilhelmi, E. de Ona A1 - Opitz, B. A1 - Ostrowski, M. A1 - Oya, I. A1 - Panter, M. A1 - Parsons, R. D. A1 - Arribas, M. Paz A1 - Pekeur, N. W. A1 - Pelletier, G. A1 - Perez, J. A1 - Petrucci, P-O A1 - Peyaud, B. A1 - Pita, S. A1 - Poon, H. A1 - Puehlhofer, G. A1 - Punch, M. A1 - Quirrenbach, A. A1 - Raab, S. A1 - Raue, M. A1 - Reimer, A. A1 - Reimer, O. A1 - Renaud, M. A1 - de los Reyes, R. A1 - Rieger, F. A1 - Rob, L. A1 - Romoli, C. A1 - Rosier-Lees, S. A1 - Rowell, G. A1 - Rudak, B. A1 - Rulten, C. B. A1 - Sahakian, V. A1 - Sanchez, David M. A1 - Santangelo, Andrea A1 - Schlickeiser, R. A1 - Schuessler, F. A1 - Schulz, A. A1 - Schwanke, U. A1 - Schwarzburg, S. A1 - Schwemmer, S. A1 - Sol, H. A1 - Spengler, G. A1 - Spies, F. A1 - Stawarz, L. A1 - Steenkamp, R. A1 - Stegmann, Christian A1 - Stinzing, F. A1 - Stycz, K. A1 - Sushch, Iurii A1 - Szostek, A. A1 - Tam, P. H. T. A1 - Tavernet, J-P A1 - Tavernier, T. A1 - Taylor, A. M. A1 - Terrier, R. A1 - Tluczykont, M. A1 - Trichard, C. A1 - Valerius, K. A1 - van Eldik, C. A1 - Vasileiadis, G. A1 - Venter, C. A1 - Viana, A. A1 - Vincent, P. A1 - Voelk, H. J. A1 - Volpe, F. A1 - Vorster, M. A1 - Wagner, S. J. A1 - Wagner, P. A1 - Ward, M. A1 - Weidinger, M. A1 - Weitzel, Q. A1 - White, R. A1 - Wierzcholska, A. A1 - Willmann, P. A1 - Woernlein, A. A1 - Wouters, D. A1 - Zacharias, M. A1 - Zajczyk, A. A1 - Zdziarski, A. A. A1 - Zech, Alraune A1 - Zechlin, H-S T1 - Search for TeV Gamma-ray emission from GRB 100621A, an extremely bright GRB in X-rays, with HESS JF - Astronomy and astrophysics : an international weekly journal N2 - The long gamma-ray burst (GRB) 100621A, at the time the brightest X-ray transient ever detected by Swift-XRT in the 0.3-10 keV range, has been observed with the H.E.S.S. imaging air Cherenkov telescope array, sensitive to gamma radiation in the very-high-energy (VHE, >100 GeV) regime. Due to its relatively small redshift of z similar to 0.5, the favourable position in the southern sky and the relatively short follow-up time (<700 s after the satellite trigger) of the H.E.S.S. observations, this GRB could be within the sensitivity reach of the HESS. instrument. The analysis of the HESS. data shows no indication of emission and yields an integral flux upper limit above similar to 380 GeV of 4.2 x 10(-12) cm(-2) s(-1) s (95% confidence level), assuming a simple Band function extension model. A comparison to a spectral-temporal model, normalised to the prompt flux at sub-MeV energies, constraints the existence of a temporally extended and strong additional hard power law, as has been observed in the other bright X-ray GRB 130427A. A comparison between the HESS. upper limit and the contemporaneous energy output in X-rays constrains the ratio between the X-ray and VHE gamma-ray fluxes to be greater than 0.4. This value is an important quantity for modelling the afterglow and can constrain leptonic emission scenarios, where leptons are responsible for the X-ray emission and might produce VHE gamma rays. KW - gamma rays: general KW - gamma-ray burst: individual: GRB 100621A KW - gamma rays: stars KW - X-rays: stars Y1 - 2014 U6 - https://doi.org/10.1051/0004-6361/201322984 SN - 0004-6361 SN - 1432-0746 VL - 565 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Goldshteyn, Jevgeni A1 - Bojahr, Andre A1 - Gaal, Peter A1 - Schick, Daniel A1 - Bargheer, Matias T1 - Selective preparation and detection of phonon polariton wavepackets by stimulated Raman scattering JF - Physica status solidi : Physica status solidi N2 - Wavevector-selective impulsive excitation of phonon-polaritons by a spectrally broad femtosecond transient grating produces wavepackets propagating in opposite directions. The photons in spectrally narrow probe pulses are scattered from these elementary excitations in lithium niobate (LiNbO3). Both elastically and inelastically scattered photons are simultaneously detected in a spectrometer. The Stokes- and anti-Stokes shifted probe pulses uniquely determine the propagation direction of the detected polariton wavepacket components and correspond to creation or annihilation of phonon-polaritons. Our experiments with spectrally broad pump and spectrally narrow probe pulses allows dissecting the four-wave-mixing process into two sequential stimulated Raman scattering events. Y1 - 2014 U6 - https://doi.org/10.1002/pssb.201350114 SN - 0370-1972 SN - 1521-3951 VL - 251 IS - 4 SP - 821 EP - 828 PB - Wiley-VCH CY - Weinheim ER - TY - JOUR A1 - Shin, Jaeoh A1 - Cherstvy, Andrey G. A1 - Metzler, Ralf T1 - Sensing viruses by mechanical tension of DNA in responsive hydrogels JF - Physical review : X, Expanding access N2 - The rapid worldwide spread of severe viral infections, often involving novel mutations of viruses, poses major challenges to our health-care systems. This means that tools that can efficiently and specifically diagnose viruses are much needed. To be relevant for broad applications in local health-care centers, such tools should be relatively cheap and easy to use. In this paper, we discuss the biophysical potential for the macroscopic detection of viruses based on the induction of a mechanical stress in a bundle of prestretched DNA molecules upon binding of viruses to the DNA. We show that the affinity of the DNA to the charged virus surface induces a local melting of the double helix into two single-stranded DNA. This process effects a mechanical stress along the DNA chains leading to an overall contraction of the DNA. Our results suggest that when such DNA bundles are incorporated in a supporting matrix such as a responsive hydrogel, the presence of viruses may indeed lead to a significant, macroscopic mechanical deformation of the matrix. We discuss the biophysical basis for this effect and characterize the physical properties of the associated DNA melting transition. In particular, we reveal several scaling relations between the relevant physical parameters of the system. We promote this DNA-based assay as a possible tool for efficient and specific virus screening. Y1 - 2014 U6 - https://doi.org/10.1103/PhysRevX.4.021002 SN - 2160-3308 VL - 4 IS - 2 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Sanders, Lloyd P. A1 - Lomholt, Michael A. A1 - Lizana, Ludvig A1 - Fogelmark, Karl A1 - Metzler, Ralf A1 - Ambjoernsson, Tobias T1 - Severe slowing-down and universality of the dynamics in disordered interacting many-body systems: ageing and ultraslow diffusion JF - New journal of physics : the open-access journal for physics N2 - Low-dimensional, many-body systems are often characterized by ultraslow dynamics. We study a labelled particle in a generic system of identical particles with hard-core interactions in a strongly disordered environment. The disorder is manifested through intermittent motion with scale-free sticking times at the single particle level. While for a non-interacting particle we find anomalous diffusion of the power-law form < x(2)(t)> similar or equal to t(alpha) of the mean squared displacement with 0 < alpha < 1, we demonstrate here that the combination of the disordered environment with the many-body interactions leads to an ultraslow, logarithmic dynamics < x(2)(t)> similar or equal to log(1/2)t with a universal 1/2 exponent. Even when a characteristic sticking time exists but the fluctuations of sticking times diverge we observe the mean squared displacement < x(2)(t)> similar or equal to t(gamma) with 0 < gamma < 1/2, that is slower than the famed Harris law < x(2)(t)> similar or equal to t(1/2) without disorder. We rationalize the results in terms of a subordination to a counting process, in which each transition is dominated by the forward waiting time of an ageing continuous time process. KW - single-file diffusion KW - continuous time random walks KW - ageing Y1 - 2014 U6 - https://doi.org/10.1088/1367-2630/16/11/113050 SN - 1367-2630 VL - 16 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Micciulla, Samantha A1 - Dodoo, Samuel A1 - Chevigny, Chloe A1 - Laschewsky, André A1 - von Klitzing, Regine T1 - Short versus long chain polyelectrolyte multilayers: a direct comparison of self-assembly and structural properties JF - Physical chemistry, chemical physics : a journal of European Chemical Societies N2 - Successful layer-by-layer (LbL) growth of short chain (similar to 30 repeat units per chain) poly(sodium styrene sulfonate) (PSS)-poly(diallyl dimethylammonium chloride) (PDADMAC) multilayers is presented for the first time and compared with the growth of equivalent long chain polyelectrolyte multilayers (PEMs). A detailed study performed by quartz crystal microbalance with dissipation (QCM-D) is carried out and three main processes are identified: (i) initial mass uptake, (ii) adsorption desorption during layer equilibration and (iii) desorption during rinsing. In contrast to the high stability and strong layer increment of high molecular weight (HMW) PEMs, layer degradation characterizes low molecular weight (LMW) multilayers. In particular, two different instability phenomena are observed: a constant decrease of sensed mass during equilibration after PDADMAC adsorption, and a strong mass toss by salt-free rinsing after PSS adsorption. Yet, an increase of salt concentration leads to much stronger layer growth. First, when the rinsing medium is changed from pure water to 0.1 M NaCl, the mass loss during rinsing is reduced, irrespective of molecular weight. Second, an increase in salt concentration in the LMW PE solutions causes a larger increment during the initial adsorption step, with no effect on the rinsing. Finally, the mechanical properties of the two systems are extracted from the measured frequency and dissipation shifts, as they offer a deeper insight into the multilayer structures depending on chain length and outermost layer. The paper enriches the field of PE assembly by presenting the use of very short PE chains to form multilayers and elucidates the role of preparation conditions to overcome the limitation of layer stability. Y1 - 2014 U6 - https://doi.org/10.1039/c4cp03439b SN - 1463-9076 SN - 1463-9084 VL - 16 IS - 40 SP - 21988 EP - 21998 PB - Royal Society of Chemistry CY - Cambridge ER - TY - INPR A1 - Gerhard, Reimund T1 - Sidney Lang - his collaboration with the University of Potsdam T2 - Ferroelectrics Y1 - 2014 U6 - https://doi.org/10.1080/00150193.2014.967090 SN - 0015-0193 SN - 1563-5112 VL - 472 IS - 1 SP - 5 EP - 5 PB - Routledge, Taylor & Francis Group CY - Abingdon ER - TY - JOUR A1 - Gerhardt, Matthias A1 - Walz, Michael A1 - Beta, Carsten T1 - Signaling in chemotactic amoebae remains spatially confined to stimulated membrane regions JF - Journal of cell science N2 - Recent work has demonstrated that the receptor-mediated signaling system in chemotactic amoeboid cells shows typical properties of an excitable system. Here, we delivered spatially confined stimuli of the chemoattractant cAMP to the membrane of differentiated Dictyostelium discoideum cells to investigate whether localized receptor stimuli can induce the spreading of excitable waves in the G-protein-dependent signal transduction system. By imaging the spatiotemporal dynamics of fluorescent markers for phosphatidylinositol (3,4,5)-trisphosphate (PIP3), PTEN and filamentous actin, we observed that the activity of the signaling pathway remained spatially confined to the stimulated membrane region. Neighboring parts of the membrane were not excited and no receptor-initiated spatial spreading of excitation waves was observed. To generate localized cAMP stimuli, either particles that carried covalently bound cAMP molecules on their surface were brought into contact with the cell or a patch of the cell membrane was aspirated into a glass micropipette to shield this patch against freely diffusing cAMP molecules in the surrounding medium. Additionally, the binding site of the cAMP receptor was probed with different surface-immobilized cAMP molecules, confirming results from earlier ligand-binding studies. KW - Signal transduction KW - Excitable dynamics KW - Dictyostelium KW - cAMP KW - PIP3 KW - PIP2 KW - PI3K KW - PTEN KW - Micropipette aspiration KW - cAMP receptor KW - Patch clamp Y1 - 2014 U6 - https://doi.org/10.1242/jcs.161133 SN - 0021-9533 SN - 1477-9137 VL - 127 IS - 23 SP - 5115 EP - 5125 PB - Company of Biologists Limited CY - Cambridge ER - TY - JOUR A1 - Di Pietro, Riccardo A1 - Venkateshvaran, Deepak A1 - Klug, Andreas A1 - List-Kratochvil, Emil J. W. A1 - Facchetti, Antonio A1 - Sirringhaus, Henning A1 - Neher, Dieter T1 - Simultaneous extraction of charge density dependent mobility and variable contact resistance from thin film transistors JF - Applied physics letters N2 - A model for the extraction of the charge density dependent mobility and variable contact resistance in thin film transistors is proposed by performing a full derivation of the current-voltage characteristics both in the linear and saturation regime of operation. The calculated values are validated against the ones obtained from direct experimental methods. This approach allows unambiguous determination of gate voltage dependent contact and channel resistance from the analysis of a single device. It solves the inconsistencies in the commonly accepted mobility extraction methods and provides additional possibilities for the analysis of the injection and transport processes in semiconducting materials. (C) 2014 AIP Publishing LLC. Y1 - 2014 U6 - https://doi.org/10.1063/1.4876057 SN - 0003-6951 SN - 1077-3118 VL - 104 IS - 19 PB - American Institute of Physics CY - Melville ER - TY - JOUR A1 - Holldack, Karsten A1 - Ovsyannikov, Ruslan A1 - Kuske, P. A1 - Mueller, R. A1 - Schaelicke, A. A1 - Scheer, M. A1 - Gorgoi, Mihaela A1 - Kuehn, D. A1 - Leitner, T. A1 - Svensson, S. A1 - Martensson, N. A1 - Föhlisch, Alexander T1 - Single bunch X-ray pulses on demand from a multi-bunch synchrotron radiation source JF - Nature Communications N2 - Synchrotron radiation facilities routinely operate in a multi-bunch regime, but applications relying on time-of-flight schemes require single bunch operation. Here we show that pulse picking by resonant excitation in a storage ring creates in addition to the multi-bunch operation a distinct and separable single bunch soft X-ray source. It has variable polarization, a photon flux of up to 10(7)-10(9) ph s(-1)/0.1%BW at purity values of 10(4)-10(2) and a repetition rate of 1.25 MHz. The quasi-resonant excitation of incoherent betatron oscillations of electrons allows horizontal pulse separation at variable (also circular) polarization accessible for both, regular 30 ps pulses and ultrashort pulses of 2-3 ps duration. Combined with a new generation of angularly resolving electron spectrometers this creates unique opportunities for time-resolved photoemission studies as confirmed by time-of-flight spectra. Our pulse picking scheme is particularly suited for surface physics at diffraction-limited light sources promising ultimate spectral resolution. Y1 - 2014 U6 - https://doi.org/10.1038/ncomms5010 SN - 2041-1723 VL - 5 PB - Nature Publ. Group CY - London ER - TY - JOUR A1 - Shalom, Menny A1 - Inal, Sahika A1 - Neher, Dieter A1 - Antonietti, Markus T1 - SiO2/carbon nitride composite materials: The role of surfaces for enhanced photocatalysis JF - Catalysis today : a serial publication dealing with topical themes in catalysis and related subjects N2 - The effect of SiO2 nanoparticles on carbon nitride (C3N4) photoactivity performance is described. The composite SiO2-C3N4 materials exhibit a higher activity in the photo degradation of RhB dye. A detailed analysis of the chemical and optical properties of the composite C3N4 materials shows that the photo activity increases with higher SiO2 concentration. We found out that the presence of SiO2 nanoparticles strongly affects the fluorescence intensity of the matrix and life time by the creation of new energy states for charge transfer within the C3N4. Furthermore, the use of SiO2 in the synthesis of C3N4 leads to new morphology with higher surface area which results in another, secondary improvement of C3N4 photoactivity. The effect of different surfaces within C3N4 on its chemical and electronic properties is discussed and a tentative mechanism is proposed. The utilization of SiO2 nanoparticles improves both photophysical and chemical properties of C3N4 and opens new possibilities for further enhancement of C3N4 catalytic properties by the formation of composites with many other materials. KW - Carbon nitride KW - SiO2 composite material KW - Photocatalysis KW - RhB degradation Y1 - 2014 U6 - https://doi.org/10.1016/j.cattod.2013.12.013 SN - 0920-5861 SN - 1873-4308 VL - 225 SP - 185 EP - 190 PB - Elsevier CY - Amsterdam ER - TY - JOUR A1 - Kliem, Bernhard A1 - Toeroek, Tibor A1 - Titov, Viacheslav S. A1 - Lionello, Roberto A1 - Linker, Jon A. A1 - Liu, Rui A1 - Liu, Chang A1 - Wang, Haimin T1 - Slow rise and partial eruption of a double-decker filament. II. A double flux rope model JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - Force-free equilibria containing two vertically arranged magnetic flux ropes of like chirality and current direction are considered as a model for split filaments/prominences and filament-sigmoid systems. Such equilibria are constructed analytically through an extension of the methods developed in Titov & Demoulin and numerically through an evolutionary sequence including shear flows, flux emergence, and flux cancellation in the photospheric boundary. It is demonstrated that the analytical equilibria are stable if an external toroidal (shear) field component exceeding a threshold value is included. If this component decreases sufficiently, then both flux ropes turn unstable for conditions typical of solar active regions, with the lower rope typically becoming unstable first. Either both flux ropes erupt upward, or only the upper rope erupts while the lower rope reconnects with the ambient flux low in the corona and is destroyed. However, for shear field strengths staying somewhat above the threshold value, the configuration also admits evolutions which lead to partial eruptions with only the upper flux rope becoming unstable and the lower one remaining in place. This can be triggered by a transfer of flux and current from the lower to the upper rope, as suggested by the observations of a split filament in Paper I. It can also result from tether-cutting reconnection with the ambient flux at the X-type structure between the flux ropes, which similarly influences their stability properties in opposite ways. This is demonstrated for the numerically constructed equilibrium. KW - instabilities KW - magnetohydrodynamics (MHD) KW - Sun: coronal mass ejections (CMEs) KW - Sun: filaments, prominences KW - Sun: flares Y1 - 2014 U6 - https://doi.org/10.1088/0004-637X/792/2/107 SN - 0004-637X SN - 1538-4357 VL - 792 IS - 2 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Maistrenko, Yuri A1 - Penkovsky, Bogdan A1 - Rosenblum, Michael T1 - Solitary state at the edge of synchrony in ensembles with attractive and repulsive interactions JF - Physical review : E, Statistical, nonlinear and soft matter physics N2 - We discuss the desynchronization transition in networks of globally coupled identical oscillators with attractive and repulsive interactions. We show that, if attractive and repulsive groups act in antiphase or close to that, a solitary state emerges with a single repulsive oscillator split up from the others fully synchronized. With further increase of the repulsing strength, the synchronized cluster becomes fuzzy and the dynamics is given by a variety of stationary states with zero common forcing. Intriguingly, solitary states represent the natural link between coherence and incoherence. The phenomenon is described analytically for phase oscillators with sine coupling and demonstrated numerically for more general amplitude models. Y1 - 2014 U6 - https://doi.org/10.1103/PhysRevE.89.060901 SN - 1539-3755 SN - 1550-2376 VL - 89 IS - 6 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Palyulin, Vladimir V. A1 - Chechkin, Aleksei V. A1 - Metzler, Ralf T1 - Space-fractional Fokker-Planck equation and optimization of random search processes in the presence of an external bias JF - Journal of statistical mechanics: theory and experiment N2 - Based on the space-fractional Fokker-Planck equation with a delta-sink term, we study the efficiency of random search processes based on Levy flights with power-law distributed jump lengths in the presence of an external drift, for instance, an underwater current, an airflow, or simply the preference of the searcher based on prior experience. While Levy flights turn out to be efficient search processes when the target is upstream relative to the starting point, in the downstream scenario, regular Brownian motion turns out to be advantageous. This is caused by the occurrence of leapovers of Levy flights, due to which Levy flights typically overshoot a point or small interval. Studying the solution of the fractional Fokker-Planck equation, we establish criteria when the combination of the external stream and the initial distance between the starting point and the target favours Levy flights over the regular Brownian search. Contrary to the common belief that Levy flights with a Levy index alpha = 1 (i.e. Cauchy flights) are optimal for sparse targets, we find that the optimal value for alpha may range in the entire interval (1, 2) and explicitly include Brownian motion as the most efficient search strategy overall. KW - driven diffusive systems (theory) KW - fluctuations (theory) KW - stochastic processes (theory) KW - diffusion Y1 - 2014 U6 - https://doi.org/10.1088/1742-5468/2014/11/P11031 SN - 1742-5468 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Aliu, E. A1 - Aune, T. A1 - Behera, B. A1 - Beilicke, M. A1 - Benbow, W. A1 - Berger, K. A1 - Bird, R. A1 - Bouvier, A. A1 - Buckley, J. H. A1 - Bugaev, V. A1 - Cerruti, M. A1 - Chen, Xuhui A1 - Ciupik, L. A1 - Connolly, M. P. A1 - Cui, W. A1 - Dumm, J. A1 - Dwarkadas, Vikram V. A1 - Errando, M. A1 - Falcone, A. A1 - Federici, Simone A1 - Feng, Q. A1 - Finley, J. P. A1 - Fleischhack, H. A1 - Fortin, P. A1 - Fortson, L. A1 - Furniss, A. A1 - Galante, N. A1 - Gillanders, G. H. A1 - Gotthelf, E. V. 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 - Kargaltsev, O. A1 - Kertzman, M. A1 - Khassen, Y. A1 - Kieda, D. A1 - Krennrich, F. A1 - Lang, M. J. A1 - Madhavan, A. S. A1 - Maier, G. A1 - McArthur, S. A1 - McCann, A. 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 - 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 - Roberts, 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 - Weinstein, A. A1 - Welsing, R. A1 - Wilhelm, Alina A1 - Williams, D. A. A1 - Zitzer, B. T1 - Spatially resolving the very high energy emission from MRGO J2019+37 wih veritas JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - We present very high energy (VHE) imaging of MGRO J2019+37 obtained with the VERITAS observatory. The bright extended (similar to 2 degrees) unidentified Milagro source is located toward the rich star formation region Cygnus-X. MGRO J2019+37 is resolved into two VERITAS sources. The faint, point-like source VER J2016+371 overlaps CTB 87, a filled-center remnant (SNR) with no evidence of a supernova remnant shell at the present time. Its spectrum is well fit in the 0.65-10 TeV energy range by a power-law model with photon index 2.3 +/- 0.4. VER J2019+378 is a bright extended (similar to 1 degrees) source that likely accounts for the bulk of the Milagro emission and is notably coincident with PSR J2021+3651 and the star formation region Sh 2-104. Its spectrum in the range 1-30 TeV is well fit with a power-law model of photon index 1.75 +/- 0.3, among the hardest values measured in the VHE band, comparable to that observed near Vela-X. We explore the unusual spectrum and morphology in the radio and X-ray bands to constrain possible emission mechanisms for this source. KW - gamma rays : stars KW - pulsars : individual (PSR J2021+3651) KW - supernovae : individual (CTB 87) Y1 - 2014 U6 - https://doi.org/10.1088/0004-637X/788/1/78 SN - 0004-637X SN - 1538-4357 VL - 788 IS - 1 PB - IOP Publ. Ltd. CY - Bristol ER - TY - INPR A1 - Hilczer, Börn A1 - Gerhard, Reimund A1 - Scott, James F. T1 - Special Issue of Ferroelectrics in Honor of S. B. Lang T2 - Ferroelectrics Y1 - 2014 U6 - https://doi.org/10.1080/00150193.2014.964099 SN - 0015-0193 SN - 1563-5112 VL - 472 IS - 1 SP - VII EP - VIII PB - Routledge, Taylor & Francis Group CY - Abingdon ER - TY - JOUR A1 - Tönjes, Ralf A1 - Sokolov, Igor M. A1 - Postnikov, Eugene B. T1 - Spectral properties of the fractional Fokker-Planck operator for the Levy flight in a harmonic potential JF - The European physical journal N2 - We present a detailed analysis of the eigenfunctions of the Fokker-Planck operator for the LevyOrnstein- Uhlenbeck process, their asymptotic behavior and recurrence relations, explicit expressions in coordinate space for the special cases of the Ornstein-Uhlenbeck process with Gaussian and with Cauchy white noise and for the transformation kernel, which maps the fractional Fokker-Planck operator of the Cauchy-Ornstein-Uhlenbeck process to the non-fractional Fokker-Planck operator of the usual Gaussian Ornstein-Uhlenbeck process. We also describe how non-spectral relaxation can be observed in bounded random variables of the Levy-Ornstein-Uhlenbeck process and their correlation functions. Y1 - 2014 U6 - https://doi.org/10.1140/epjb/e2014-50558-5 SN - 1434-6028 SN - 1434-6036 VL - 87 IS - 12 PB - Springer CY - New York ER - TY - JOUR A1 - Palyulin, Vladimir V. A1 - Metzler, Ralf T1 - Speeding up the first-passage for subdiffusion by introducing a finite potential barrier JF - Journal of physics : A, Mathematical and theoretical N2 - We show that for a subdiffusive continuous time random walk with scale-free waiting time distribution the first-passage dynamics on a finite interval can be optimized by introduction of a piecewise linear potential barrier. Analytical results for the survival probability and first-passage density based on the fractional Fokker-Planck equation are shown to agree well with Monte Carlo simulations results. As an application we discuss an improved design for efficient translocation of gradient copolymers compared to homopolymer translocation in a quasi-equilibrium approximation. KW - first passage KW - anomalous diffusion KW - potential landscape KW - polymer translocation Y1 - 2014 U6 - https://doi.org/10.1088/1751-8113/47/3/032002 SN - 1751-8113 SN - 1751-8121 VL - 47 IS - 3 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Albrecht, Torsten A1 - Levermann, Anders T1 - Spontaneous ice-front retreat caused by disintegration of adjacent ice shelf in Antarctica JF - Earth & planetary science letters N2 - Antarctic ice-discharge constitutes the largest uncertainty in future sea-level projections. Floating ice shelves, fringing most of Antarctica, exert retentive forces onto the ice flow. While abrupt ice-shelf retreat has been observed, it is generally considered a localized phenomenon. Here we show that the disintegration of an ice shelf may induce the spontaneous retreat of its neighbor. As an example, we reproduce the spontaneous but gradual retreat of the Larsen B ice front as observed after the disintegration of the adjacent Larsen A ice shelf. We show that the Larsen A collapse yields a change in spreading rate in Larsen B via their connecting ice channels and thereby causes a retreat of the ice front to its observed position of the year 2000, prior to its collapse. This mechanism might be particularly relevant for the role of East Antarctica and the Antarctic Peninsula in future sea level. KW - Antarctica KW - Larsen Ice Shelf KW - glaciology KW - numerical ice modeling KW - sea level KW - iceberg calving Y1 - 2014 U6 - https://doi.org/10.1016/j.epsl.2014.02.034 SN - 0012-821X SN - 1385-013X VL - 393 SP - 26 EP - 30 PB - Elsevier CY - Amsterdam ER - TY - JOUR A1 - Miedema, Piter S. A1 - Wernet, Philippe A1 - Föhlisch, Alexander T1 - State-dependent fluorescence yields through the core-valence Coulomb exchange parameter JF - Physical review : A, Atomic, molecular, and optical physics N2 - Total and partial fluorescence yield (PFY) L-edge x-ray absorption spectra differ from the transmission x-ray absorption spectra (XAS) through state-dependent fluorescence yield across the XAS. For 3d(1) to 3d(9) in octahedral symmetry we apply simulations of PFY and XAS and show how the atomic 2p3d Coulomb exchange parameter G(pd) governs the differences in the L-3/(L-2 + L-3) branching ratio between PFY and XAS. G(pd) orders the XAS final states following Hund's rules creating a strong state-dependent fluorescence decay strength variation across the XAS leading to the differences between PFY and XAS. Y1 - 2014 U6 - https://doi.org/10.1103/PhysRevA.89.052507 SN - 1050-2947 SN - 1094-1622 VL - 89 IS - 5 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Winkler, Roland G. A1 - Cherstvy, Andrey G. ED - Muller, M. T1 - Strong and weak polyelectrolyte adsorption onto oppositely charged curved surfaces JF - Advances in polymer science JF - Advances in Polymer Science N2 - Polyelectrolytes are macromolecules composed of charged monomers and exhibit unique properties due to the interplay of their flexibility and electrostatic interactions. In solution, they are attracted to oppositely charged surfaces and interfaces and exhibit a transition to an adsorbed state when certain conditions are met concerning the charge densities of the polymer and surface and the properties of the solution. In this review, we discuss two limiting cases for adsorption of flexible polyelectrolytes on curved surfaces: weak and strong adsorption. In the first case, adsorption is strongly influenced by the entropic degrees of freedom of a flexible polyelectrolyte. By contrast, in the strong adsorption limit, electrostatic interactions dominate, which leads to particular adsorption patterns, specifically on spherical surfaces. We discuss the corresponding theoretical approaches, applying a mean-field description for the polymer and the polymer-surface interaction. For weak adsorption, we discuss the critical adsorption behavior by exactly solvable models for planar and spherical geometries and a generic approximation scheme, which is additionally applied to cylindrical surfaces. For strong adsorption, we investigate various polyelectrolyte patterns on cylinders and spheres and evaluate their stability. The results are discussed in the light of experimental results, mostly of DNA adsorption experiments. Y1 - 2014 SN - 978-3-642-40734-5; 978-3-642-40733-8 U6 - https://doi.org/10.1007/12_2012_183 SN - 0065-3195 VL - 255 SP - 1 EP - 56 PB - Springer CY - Berlin ER - TY - JOUR A1 - Joulain, Karl A1 - Ben-Abdallah, Philippe A1 - Chapuis, Pierre-Olivier A1 - De Wilde, Y. A1 - Babuty, A. A1 - Henkel, Carsten T1 - Strong tip-sample coupling in thermal radiation scanning tunneling microscopy JF - Journal of quantitative spectroscopy & radiative transfer KW - Near-field thermal radiation KW - Infrared radiation KW - Local density of states KW - Scanning near-field optical microscopy KW - Tip-sample interactions KW - Local spectroscopy Y1 - 2014 U6 - https://doi.org/10.1016/j.jqsrt.2013.12.006 SN - 0022-4073 SN - 1879-1352 VL - 136 SP - 1 EP - 15 PB - Elsevier CY - Oxford ER - TY - JOUR A1 - Louis, Rohan E. A1 - Puschmann, Klaus G. A1 - Kliem, Bernhard A1 - Balthasar, Horst A1 - Denker, Carsten T1 - Sunspot splitting triggering an eruptive flare JF - Astronomy and astrophysics : an international weekly journal N2 - Aims. We investigate how the splitting of the leading sunspot and associated flux emergence and cancellation in active region NOAA 11515 caused an eruptive M5.6 flare on 2012 July 2. Methods. Continuum intensity, line-of-sight magnetogram, and dopplergram data of the Helioseismic and Magnetic Imager were employed to analyse the photospheric evolution. Filtergrams in H alpha and He I 10830 angstrom of the Chromospheric Telescope at the Observatorio del Teide, Tenerife, track the evolution of the flare. The corresponding coronal conditions were derived from 171 angstrom and 304 angstrom images of the Atmospheric Imaging Assembly. Local correlation tracking was utilized to determine shear flows. Results. Emerging flux formed a neutral line ahead of the leading sunspot and new satellite spots. The sunspot splitting caused a long-lasting flow towards this neutral line, where a filament formed. Further flux emergence, partly of mixed polarity, as well as episodes of flux cancellation occurred repeatedly at the neutral line. Following a nearby C-class precursor flare with signs of interaction with the filament, the filament erupted nearly simultaneously with the onset of the M5.6 flare and evolved into a coronal mass ejection. The sunspot stretched without forming a light bridge, splitting unusually fast (within about a day, complete approximate to 6 h after the eruption) in two nearly equal parts. The front part separated strongly from the active region to approach the neighbouring active region where all its coronal magnetic connections were rooted. It also rotated rapidly (by 4.9 degrees h(-1)) and caused significant shear flows at its edge. Conclusions. The eruption resulted from a complex sequence of processes in the (sub-)photosphere and corona. The persistent flows towards the neutral line likely caused the formation of a flux rope that held the filament. These flows, their associated flux cancellation, the emerging flux, and the precursor flare all contributed to the destabilization of the flux rope. We interpret the sunspot splitting as the separation of two flux bundles differently rooted in the convection zone and only temporarily joined in the spot. This explains the rotation as the continued rise of the separating flux, and it implies that at least this part of the sunspot was still connected to its roots deep in the convection zone. KW - Sun: flares KW - sunspots KW - Sun: photosphere KW - Sun: chromosphere KW - techniques: photometric Y1 - 2014 U6 - https://doi.org/10.1051/0004-6361/201321106 SN - 0004-6361 SN - 1432-0746 VL - 562 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Vlasov, Vladimir A1 - Macau, Elbert E. N. A1 - Pikovskij, Arkadij T1 - Synchronization of oscillators in a Kuramoto-type model with generic coupling JF - Chaos : an interdisciplinary journal of nonlinear science N2 - We study synchronization properties of coupled oscillators on networks that allow description in terms of global mean field coupling. These models generalize the standard Kuramoto-Sakaguchi model, allowing for different contributions of oscillators to the mean field and to different forces from the mean field on oscillators. We present the explicit solutions of self-consistency equations for the amplitude and frequency of the mean field in a parametric form, valid for noise-free and noise-driven oscillators. As an example, we consider spatially spreaded oscillators for which the coupling properties are determined by finite velocity of signal propagation. (C) 2014 AIP Publishing LLC. Y1 - 2014 U6 - https://doi.org/10.1063/1.4880835 SN - 1054-1500 SN - 1089-7682 VL - 24 IS - 2 PB - American Institute of Physics CY - Melville ER - TY - JOUR A1 - Komarov, Maxim A1 - Gupta, Shamik A1 - Pikovskij, Arkadij T1 - Synchronization transitions in globally coupled rotors in the presence of noise and inertia: Exact results JF - epl : a letters journal exploring the frontiers of physics N2 - We study a generic model of globally coupled rotors that includes the effects of noise, phase shift in the coupling, and distributions of moments of inertia and natural frequencies of oscillation. As particular cases, the setup includes previously studied Sakaguchi-Kuramoto, Hamiltonian and Brownian mean-field, and Tanaka-Lichtenberg-Oishi and Acebron-Bonilla-Spigler models. We derive an exact solution of the self-consistent equations for the order parameter in the stationary state, valid for arbitrary parameters in the dynamics, and demonstrate nontrivial phase transitions to synchrony that include reentrant synchronous regimes. Copyright (C) EPLA, 2014 Y1 - 2014 U6 - https://doi.org/10.1209/0295-5075/106/40003 SN - 0295-5075 SN - 1286-4854 VL - 106 IS - 4 PB - EDP Sciences CY - Mulhouse ER - TY - JOUR A1 - Zhang, Haocheng A1 - Chen, Xuhui A1 - Boettcher, Markus T1 - Synchrotron polarization in blazars JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - We present a detailed analysis of time-and energy-dependent synchrotron polarization signatures in a shock-in-jet model for gamma-ray blazars. Our calculations employ a full three-dimensional radiation transfer code, assuming a helical magnetic field throughout the jet. The code considers synchrotron emission from an ordered magnetic field, and takes into account all light-travel-time and other relevant geometric effects, while the relevant synchrotron self-Compton and external Compton effects are handled with the two-dimensional Monte-Carlo/Fokker-Planck (MCFP) code. We consider several possible mechanisms through which a relativistic shock propagating through the jet may affect the jet plasma to produce a synchrotron and high-energy flare. Most plausibly, the shock is expected to lead to a compression of the magnetic field, increasing the toroidal field component and thereby changing the direction of the magnetic field in the region affected by the shock. We find that such a scenario leads to correlated synchrotron + synchrotron-self-Compton flaring, associated with substantial variability in the synchrotron polarization percentage and position angle. Most importantly, this scenario naturally explains large polarization angle rotations by greater than or similar to 180 degrees, as observed in connection with gamma-ray flares in several blazars, without the need for bent or helical jet trajectories or other nonaxisymmetric jet features. KW - galaxies: active KW - galaxies: jets KW - gamma rays: galaxies KW - radiation mechanisms: non-thermal KW - relativistic processes Y1 - 2014 U6 - https://doi.org/10.1088/0004-637X/789/1/66 SN - 0004-637X SN - 1538-4357 VL - 789 IS - 1 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Meibohm, Jan A1 - Schreck, Simon A1 - Wernet, Philippe T1 - Temperature dependent soft x-ray absorption spectroscopy of liquids JF - Review of scientific instruments : a monthly journal devoted to scientific instruments, apparatus, and techniques N2 - A novel sample holder is introduced which allows for temperature dependent soft x-ray absorption spectroscopy of liquids in transmission mode. The setup is based on sample cells with x-ray transmissive silicon nitride windows. A cooling circuit allows for temperature regulation of the sample liquid between -10 degrees C and +50 degrees C. The setup enables to record soft x-ray absorption spectra of liquids in transmission mode with a temperature resolution of 0.5K and better. Reliability and reproducibility of the spectra are demonstrated by investigating the characteristic temperature-induced changes in the oxygen K-edge x-ray absorption spectrum of liquid water. These are compared to the corresponding changes in the oxygen K-edge spectra from x-ray Raman scattering. (C) 2014 AIP Publishing LLC. Y1 - 2014 U6 - https://doi.org/10.1063/1.4896977 SN - 0034-6748 SN - 1089-7623 VL - 85 IS - 10 PB - American Institute of Physics CY - Melville 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 - Abramowski, Attila A1 - Aharonian, Felix A. A1 - Benkhali, Faical Ait A1 - Akhperjanian, A. G. A1 - Angüner, Ekrem Oǧuzhan A1 - Anton, Gisela A1 - Balenderan, Shangkari A1 - Balzer, Arnim A1 - Barnacka, Anna A1 - Becherini, Yvonne A1 - Tjus, J. Becker A1 - Bernlöhr, K. A1 - Birsin, E. A1 - Bissaldi, E. A1 - Biteau, Jonathan A1 - Boettcher, Markus A1 - Boisson, Catherine A1 - Bolmont, J. A1 - Bordas, Pol A1 - Brucker, J. A1 - Brun, Francois A1 - Brun, Pierre A1 - Bulik, Tomasz A1 - Carrigan, Svenja A1 - Casanova, Sabrina A1 - Cerruti, M. A1 - Chadwick, Paula M. A1 - Chalme-Calvet, R. A1 - Chaves, Ryan C. G. A1 - Cheesebrough, A. A1 - Chretien, M. A1 - Colafrancesco, Sergio A1 - Cologna, Gabriele A1 - Conrad, Jan A1 - Couturier, C. A1 - Cui, Y. A1 - Dalton, M. A1 - Daniel, M. K. A1 - Davids, I. D. A1 - Degrange, B. A1 - Deil, C. A1 - deWilt, P. A1 - Dickinson, H. J. A1 - Djannati-Ataï, A. A1 - Domainko, W. A1 - Dubus, G. A1 - Dutson, K. A1 - Dyks, J. A1 - Dyrda, M. A1 - Edwards, T. A1 - Egberts, Kathrin A1 - Eger, P. A1 - Espigat, P. A1 - Farnier, C. A1 - Fegan, S. A1 - Feinstein, F. A1 - Fernandes, M. V. A1 - Fernandez, D. A1 - Fiasson, A. A1 - Fontaine, G. A1 - Foerster, A. A1 - Fuessling, Matthias A1 - Gajdus, M. A1 - Gallant, Y. A. A1 - Garrigoux, T. A1 - Giavitto, G. A1 - Giebels, B. A1 - Glicenstein, J. F. A1 - Grondin, M. -H. A1 - Grudzinska, M. A1 - Haeffner, S. A1 - Hahn, J. A1 - Harris, J. A1 - Heinzelmann, G. A1 - Henri, G. A1 - Hermann, G. A1 - Hervet, O. A1 - Hillert, A. A1 - Hinton, James Anthony A1 - Hofmann, W. A1 - Hofverberg, P. A1 - Holler, M. A1 - Horns, D. A1 - Jacholkowska, A. A1 - Jahn, C. A1 - Jamrozy, M. A1 - Janiak, M. A1 - Jankowsky, F. A1 - Jung, I. A1 - Kastendieck, M. A. A1 - Katarzynski, K. A1 - Katz, U. A1 - Kaufmann, S. A1 - Khelifi, B. A1 - Kieffer, M. A1 - Klepser, S. A1 - Klochkov, D. A1 - Kluzniak, W. A1 - Kneiske, T. A1 - Kolitzus, D. A1 - Komin, Nu A1 - Kosack, K. A1 - Krakau, S. A1 - Krayzel, F. A1 - Krueger, P. P. A1 - Laffon, H. A1 - Lamanna, G. A1 - Lefaucheur, J. A1 - Lemiere, A. A1 - Lemoine-Goumard, M. A1 - Lenain, J. -P. A1 - Lennarz, D. A1 - Lohse, T. A1 - Lopatin, A. A1 - Lu, C. -C. A1 - Marandon, V. A1 - Marcowith, Alexandre A1 - Marx, R. A1 - Maurin, G. A1 - Maxted, N. A1 - Mayer, M. A1 - McComb, T. J. L. A1 - Mehault, J. A1 - Meintjes, P. J. A1 - Menzler, U. A1 - Meyer, M. A1 - Moderski, R. A1 - Mohamed, M. A1 - Moulin, Emmanuel A1 - Murach, T. A1 - Naumann, C. L. A1 - de Naurois, M. A1 - Niemiec, J. A1 - Nolan, S. J. A1 - Oakes, L. A1 - Ohm, S. A1 - Wilhelmi, E. de Ona A1 - Opitz, B. A1 - Ostrowski, M. A1 - Oya, I. A1 - Panter, M. A1 - Parsons, R. D. A1 - Arribas, M. Paz A1 - Pekeur, N. W. A1 - Pelletier, G. A1 - Perez, J. A1 - Petrucci, P. -O. A1 - Peyaud, B. A1 - Pita, S. A1 - Poon, H. A1 - Puehlhofer, G. A1 - Punch, M. A1 - Quirrenbach, A. A1 - Raab, S. A1 - Raue, M. A1 - Reimer, A. A1 - Reimer, O. A1 - Renaud, M. A1 - de los Reyes, R. A1 - Rieger, F. A1 - Rob, L. A1 - Romoli, C. A1 - Rosier-Lees, S. A1 - Rowell, G. A1 - Rudak, B. A1 - Rulten, C. B. A1 - Sahakian, V. A1 - Sanchez, David M. A1 - Santangelo, Andrea A1 - Schlickeiser, R. A1 - Schuessler, F. A1 - Schulz, A. A1 - Schwanke, U. A1 - Schwarzburg, S. A1 - Schwemmer, S. A1 - Sol, H. A1 - Spengler, G. A1 - Spies, F. A1 - Stawarz, L. A1 - Steenkamp, R. A1 - Stegmann, Christian A1 - Stinzing, F. A1 - Stycz, K. A1 - Sushch, Iurii A1 - Szostek, A. A1 - Tavernet, J. -P. A1 - Tavernier, T. A1 - Taylor, A. M. A1 - Terrier, R. A1 - Tluczykont, M. A1 - Trichard, C. A1 - Valerius, K. A1 - van Eldik, C. A1 - van Soelen, B. A1 - Vasileiadis, G. A1 - Venter, C. A1 - Viana, A. A1 - Vincent, P. A1 - Voelk, H. J. A1 - Volpe, F. A1 - Vorster, M. A1 - Vuillaume, T. A1 - Wagner, S. J. A1 - Wagner, P. A1 - Ward, M. A1 - Weidinger, M. A1 - Weitzel, Q. A1 - White, R. A1 - Wierzcholska, A. A1 - Willmann, P. A1 - Woernlein, A. A1 - Wouters, D. A1 - Zabalza, V. A1 - Zacharias, M. A1 - Zajczyk, A. A1 - Zdziarski, A. A. A1 - Zech, Alraune A1 - Zechlin, H. -S. T1 - TeV gamma-ray observations of the young synchrotron-dominated SNRs G1.9+0.3 and G330.2+1.0 with HESS JF - Monthly notices of the Royal Astronomical Society N2 - The non-thermal nature of the X-ray emission from the shell-type supernova remnants (SNRs) G1.9+0.3 and G330.2+1.0 is an indication of intense particle acceleration in the shock fronts of both objects. This suggests that the SNRs are prime candidates for very-high-energy (VHE; E > 0.1 TeV) gamma-ray observations. G1.9+0.3, recently established as the youngest known SNR in the Galaxy, also offers a unique opportunity to study the earliest stages of SNR evolution in the VHE domain. The purpose of this work is to probe the level of VHE gamma-ray emission from both SNRs and use this to constrain their physical properties. Observations were conducted with the H. E. S. S. (High Energy Stereoscopic System) Cherenkov Telescope Array over a more than six-year period spanning 2004-2010. The obtained data have effective livetimes of 67 h for G1.9+0.3 and 16 h for G330.2+1.0. The data are analysed in the context of the multiwavelength observations currently available and in the framework of both leptonic and hadronic particle acceleration scenarios. No significant gamma-ray signal from G1.9+0.3 or G330.2+1.0 was detected. Upper limits (99 per cent confidence level) to the TeV flux from G1.9+0.3 and G330.2+1.0 for the assumed spectral index Gamma = 2.5 were set at 5.6 x 10(-1)3 cm(-2) s(-1) above 0.26 TeV and 3.2 x 10(-12) cm(-2) s(-1) above 0.38 TeV, respectively. In a one-zone leptonic scenario, these upper limits imply lower limits on the interior magnetic field to B-G1.9 greater than or similar to 12 mu G for G1.9+0.3 and to B-G330 greater than or similar to 8 mu G for G330.2+1.0. In a hadronic scenario, the low ambient densities and the large distances to the SNRs result in very low predicted fluxes, for which the H.E.S.S. upper limits are not constraining. KW - radiation mechanisms: non-thermal KW - ISM: individual objects: SNR G1.9+0.3 KW - ISM: individual objects: SNR G330.2+1.0 KW - ISM: magnetic fields KW - ISM: supernova remnants KW - gamma-rays: ISM Y1 - 2014 U6 - https://doi.org/10.1093/mnras/stu459 SN - 0035-8711 SN - 1365-2966 VL - 441 IS - 1 SP - 790 EP - 799 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Miedema, P. S. A1 - Beye, Martin A1 - Koennecke, R. A1 - Schiwietz, G. A1 - Föhlisch, Alexander T1 - The angular- and crystal-momentum transfer through electron-phonon coupling in silicon and silicon-carbide: similarities and differences JF - New journal of physics : the open-access journal for physics N2 - Electron-phonon scattering has been studied for silicon carbide (6H-SiC) with resonant inelastic x-ray scattering at the silicon 2p edge. The observed electron-phonon scattering yields a crystal momentum transfer rate per average phonon in 6H-SiC of 1.8 fs(-1) while it is 0.2 fs(-1) in crystalline silicon. The angular momentum transfer rate per average phonon for 6H-SiC is 0.1 fs(-1), which is much higher than 0.0035 fs(-1) obtained for crystalline silicon in a previous study. The higher electron-phonon scattering rates in 6H-SiC are a result of the larger electron localization at the silicon atoms in 6H-SiC as compared to crystalline silicon. While delocalized valence electrons can screen effectively (part of) the electron-phonon interaction, this effect is suppressed for 6H-SiC in comparison to crystalline silicon. Smaller contributions to the difference in electron-phonon scattering rates between 6H-SiC and silicon arise from the lower atomic mass of carbon versus silicon and the difference in local symmetry. KW - electron-phonon scattering KW - 6H-SiC KW - RIXS Y1 - 2014 U6 - https://doi.org/10.1088/1367-2630/16/9/093056 SN - 1367-2630 VL - 16 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Zaritsky, Dennis A1 - Courtois, Helene A1 - Munoz-Mateos, Juan-Carlos A1 - Sorce, Jenny A1 - Erroz-Ferrer, S. A1 - Comeron, S. A1 - Gadotti, D. A. A1 - Gil De Paz, A. A1 - Hinz, J. L. A1 - Laurikainen, E. A1 - Kim, T. A1 - Laine, J. A1 - Menendez-Delmestre, K. A1 - Mizusawa, T. A1 - Regan, M. W. A1 - Salo, H. A1 - Seibert, M. A1 - Sheth, K. A1 - Athanassoula, E. A1 - Bosma, A. A1 - Cisternas, M. A1 - Ho, Luis C. A1 - Holwerda, B. T1 - The baryonic Tully-Fisher relationship for S(4)G galaxies and the "condensed" baryon fraction of galaxies JF - The astronomical journal N2 - We combine data from the Spitzer Survey for Stellar Structure in Galaxies, a recently calibrated empirical stellar mass estimator from Eskew et al., and an extensive database of Hi spectral line profiles to examine the baryonic Tully-Fisher (BTF) relation. We find (1) that the BTF has lower scatter than the classic Tully-Fisher (TF) relation and is better described as a linear relationship, confirming similar previous results, (2) that the inclusion of a radial scale in the BTF decreases the scatter but only modestly, as seen previously for the TF relation, and (3) that the slope of the BTF, which we find to be 3.5 +/- 0.2 (Delta log M-baryon/Delta log v(c)), implies that on average a nearly constant fraction (similar to 0.4) of all baryons expected to be in a halo are "condensed" onto the central region of rotationally supported galaxies. The condensed baryon fraction, M-baryon/M-total, is, to our measurement precision, nearly independent of galaxy circular velocity (our sample spans circular velocities, vc, between 60 and 250 km s(-1), but is extended to v(c) similar to 10 km s(-1) using data from the literature). The observed galaxy-to-galaxy scatter in this fraction is generally <= a factor of 2 despite fairly liberal selection criteria. These results imply that cooling and heating processes, such as cold versus hot accretion, mass loss due to stellar winds, and active galactic nucleus driven feedback, to the degree that they affect the global galactic properties involved in the BTF, are independent of halo mass for galaxies with 10 < v(c) < 250 km s(-1) and typically introduce no more than a factor of two range in the resulting M-baryon/M-total. Recent simulations by Aumer et al. of a small sample of disk galaxies are in excellent agreement with our data, suggesting that current simulations are capable of reproducing the global properties of individual disk galaxies. More detailed comparison to models using the BTF holds great promise, but awaits improved determinations of the stellar masses. KW - galaxies: evolution KW - galaxies: formation KW - galaxies: fundamental parameters KW - galaxies: stellar content KW - galaxies: structure Y1 - 2014 U6 - https://doi.org/10.1088/0004-6256/147/6/134 SN - 0004-6256 SN - 1538-3881 VL - 147 IS - 6 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Fox, Andrew J. A1 - Wakker, Bart P. A1 - Barger, Kathleen A. A1 - Hernandez, Audra K. A1 - Richter, Philipp A1 - Lehner, Nicolas A1 - Bland-Hawthorn, Joss A1 - Charlton, Jane C. A1 - Westmeier, Tobias A1 - Thom, Christopher A1 - Tumlinson, Jason A1 - Misawa, Toru A1 - Howk, J. Christopher A1 - Haffner, L. Matthew A1 - Ely, Justin A1 - Rodriguez-Hidalgo, Paola A1 - Kumari, Nimisha T1 - The COS/UVES absorption survey of the magellanic stream. III. Ionization, total mass, and inflow rate onto the milky way JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - Dynamic interactions between the two Magellanic Clouds have flung large quantities of gas into the halo of the Milky Way. The result is a spectacular arrangement of gaseous structures, including the Magellanic Stream, the Magellanic Bridge, and the Leading Arm (collectively referred to as the Magellanic System). In this third paper of a series studying the Magellanic gas in absorption, we analyze the gas ionization level using a sample of 69 Hubble Space Telescope/Cosmic Origins Spectrograph sightlines that pass through or within 30 degrees of the 21 cm emitting regions. We find that 81% (56/69) of the sightlines show UV absorption at Magellanic velocities, indicating that the total cross-section of the Magellanic System is approximate to 11,000 deg(2), or around one-quarter of the entire sky. Using observations of the Si III/Si II ratio together with Cloudy photoionization modeling, we calculate the total gas mass (atomic plus ionized) of the Magellanic System to be approximate to 2.0 x 10(9) M-circle dot (d/55 kpc)(2), with the ionized gas contributing around three times as much mass as the atomic gas. This is larger than the current-day interstellar H I mass of both Magellanic Clouds combined, indicating that they have lost most of their initial gas mass. If the gas in the Magellanic System survives to reach the Galactic disk over its inflow time of similar to 0.5-1.0 Gyr, it will represent an average inflow rate of similar to 3.7-6.7 M-circle dot yr(-1), potentially raising the Galactic star formation rate. However, multiple signs of an evaporative interaction with the hot Galactic corona indicate that the Magellanic gas may not survive its journey to the disk fully intact and will instead add material to (and cool) the corona. KW - Galaxy: evolution KW - Galaxy: halo KW - ISM: abundances KW - Magellanic Clouds KW - quasars: absorption lines Y1 - 2014 U6 - https://doi.org/10.1088/0004-637X/787/2/147 SN - 0004-637X SN - 1538-4357 VL - 787 IS - 2 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Nuza, Sebastian E. A1 - Parisi, Florencia A1 - Scannapieco, Cecilia A1 - Richter, Philipp A1 - Gottloeber, Stefan A1 - Steinmetz, Matthias T1 - The distribution of gas in the Local Group from constrained cosmological simulations: the case for Andromeda and the Milky Way galaxies JF - Monthly notices of the Royal Astronomical Society N2 - We study the gas distribution in the Milky Way and Andromeda using a constrained cosmological simulation of the Local Group (LG) within the context of the CLUES (Constrained Local UniversE Simulations) project. We analyse the properties of gas in the simulated galaxies at z = 0 for three different phases: 'cold', 'hot' and H i, and compare our results with observations. The amount of material in the hot halo (M-hot a parts per thousand 4-5 x 10(10) M-aS (TM)), and the cold (M-cold(r a parts per thousand(2) 10 kpc) a parts per thousand 10(8) M-aS (TM)) and H i components displays reasonable agreement with observations. We also compute the accretion/ejection rates together with the H i (radial and all-sky) covering fractions. The integrated H i accretion rate within r = 50 kpc gives similar to 0.2-0.3 M-aS (TM) yr(-1), i.e. close to that obtained from high-velocity clouds in the Milky Way. We find that the global accretion rate is dominated by hot material, although ionized gas with T a parts per thousand(2) 10(5) K can contribute significantly too. The net accretion rates of all material at the virial radii are 6-8 M-aS (TM) yr(-1). At z = 0, we find a significant gas excess between the two galaxies, as compared to any other direction, resulting from the overlap of their gaseous haloes. In our simulation, the gas excess first occurs at z similar to 1, as a result of the kinematical evolution of the LG. KW - methods: numerical KW - Galaxy: halo KW - intergalactic medium KW - Local Group KW - large-scale structure of Universe Y1 - 2014 U6 - https://doi.org/10.1093/mnras/stu643 SN - 0035-8711 SN - 1365-2966 VL - 441 IS - 3 SP - 2593 EP - 2612 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Toeroek, T. A1 - Kliem, Bernhard A1 - Berger, M. A. A1 - Linton, M. G. A1 - Demoulin, Pascal A1 - van Driel-Gesztelyi, L. T1 - The evolution of writhe in kink-unstable flux ropes and erupting filaments JF - Plasma physics and controlled fusion N2 - The helical kink instability of a twisted magnetic flux tube has been suggested as a trigger mechanism for solar filament eruptions and coronal mass ejections (CMEs). In order to investigate if estimations of the pre-emptive twist can be obtained from observations of writhe in such events, we quantitatively analyze the conversion of twist into writhe in the course of the instability, using numerical simulations. We consider the line tied, cylindrically symmetric Gold-Hoyle flux rope model and measure the writhe using the formulae by Berger and Prior which express the quantity as a single integral in space. We find that the amount of twist converted into writhe does not simply scale with the initial flux rope twist, but depends mainly on the growth rates of the instability eigenmodes of higher longitudinal order than the basic mode. The saturation levels of the writhe, as well as the shapes of the kinked flux ropes, are very similar for considerable ranges of initial flux rope twists, which essentially precludes estimations of pre-eruptive twist from measurements of writhe. However, our simulations suggest an upper twist limit of similar to 6 pi for the majority of filaments prior to their eruption. KW - magnetohydrodynamics (MHD) KW - Sun: corona KW - Sun: filaments Y1 - 2014 U6 - https://doi.org/10.1088/0741-3335/56/6/064012 SN - 0741-3335 SN - 1361-6587 VL - 56 IS - 6 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Balzer, Arnim A1 - Fuessling, M. A1 - Gajdus, M. A1 - Goering, D. A1 - Lopatin, A. A1 - de Naurois, M. A1 - Schlenker, S. A1 - Schwanke, U. A1 - Stegmann, Christian T1 - The HESS central data acquisition system JF - Astroparticle physics KW - DAQ KW - Data acquisition KW - VHE KW - Gamma ray astronomy KW - HESS Y1 - 2014 U6 - https://doi.org/10.1016/j.astropartphys.2013.11.007 SN - 0927-6505 SN - 1873-2852 VL - 54 SP - 67 EP - 80 PB - Elsevier CY - Amsterdam ER - TY - JOUR A1 - Shenar, Tomer A1 - Hamann, Wolf-Rainer A1 - Todt, Helge Tobias T1 - The impact of rotation on the line profiles of Wolf-Rayet stars JF - Astronomy and astrophysics : an international weekly journal N2 - Context. Massive Wolf-Rayet stars are recognized today to be in a very common, but short, evolutionary phase of massive stars. While our understanding of Wolf-Rayet stars has increased dramatically over the past decades, it remains unclear whether rapid rotators are among them. There are various indications that rapidly rotating Wolf-Rayet stars should exist. Unfortunately, due to their expanding atmospheres, rotational velocities of Wolf-Rayet stars are very difficult to measure. However, recently observed spectra of several Wolf-Rayet stars reveal peculiarly broad and round emission lines. Could these spectra imply rapid rotation? Aims. In this work, we model the effects of rotation on the atmospheres of Wolf-Rayet stars. We further investigate whether the peculiar spectra of five Wolf-Rayet stars may be explained with the help of stellar rotation, infer appropriate rotation parameters, and discuss the implications of our results. Methods. We make use of the Potsdam Wolf-Rayet (PoWR) non-LTE model atmosphere code. Since the observed spectra of WolfRayet stars are mainly formed in their expanding atmospheres, rotation must be accounted for with a 3D integration scheme of the formal integral. For this purpose, we assume a rotational velocity field consisting of an inner co-rotating domain and an outer domain, where the angular momentum is conserved. Results. We find that rotation can reproduce the unique spectra analyzed here. However, the inferred rotational velocities at the stellar surface are large (similar to 200 km s(-1)), and the inferred co-rotation radii (similar to 10R.) suggest the existence of very strong photospheric magnetic fields (similar to 20 kG). KW - stars: Wolf-Rayet KW - Magellanic Clouds KW - stars: magnetic field KW - stars: massive KW - gamma-ray burst: general KW - stars: rotation Y1 - 2014 U6 - https://doi.org/10.1051/0004-6361/201322496 SN - 0004-6361 SN - 1432-0746 VL - 562 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Komarov, Maxim A1 - Pikovskij, Arkadij T1 - The Kuramoto model of coupled oscillators with a bi-harmonic coupling function JF - Physica : D, Nonlinear phenomena N2 - We study synchronization in a Kuramoto model of globally coupled phase oscillators with a bi-harmonic coupling function, in the thermodynamic limit of large populations. We develop a method for an analytic solution of self-consistent equations describing uniformly rotating complex order parameters, both for single-branch (one possible state of locked oscillators) and multi-branch (two possible values of locked phases) entrainment. We show that synchronous states coexist with the neutrally linearly stable asynchronous regime. The latter has a finite life time for finite ensembles, this time grows with the ensemble size as a power law. (C) 2014 Elsevier B.V. All rights reserved. KW - Kuramoto model KW - Bi-harmonic coupling function KW - Multi-branch entrainment KW - Synchronization Y1 - 2014 U6 - https://doi.org/10.1016/j.physd.2014.09.002 SN - 0167-2789 SN - 1872-8022 VL - 289 SP - 18 EP - 31 PB - Elsevier CY - Amsterdam ER - TY - GEN A1 - Liermann, Angelika A1 - Hamann, Wolf-Rainer A1 - Oskinova, Lidia M. T1 - The quintuplet cluster III. Hertzsprung-Russell diagram and cluster age (vol 540, pg A14, 2012) T2 - Astronomy and astrophysics : an international weekly journal KW - open clusters and associations: individual: Quintuplet KW - infrared: stars KW - stars: early-type KW - stars: late-type KW - Hertzsprung-Russell and C-M diagrams KW - errata, addenda Y1 - 2014 U6 - https://doi.org/10.1051/0004-6361/201117534e SN - 0004-6361 SN - 1432-0746 VL - 563 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Reindl, Nicole A1 - Rauch, Thomas A1 - Parthasarathy, M. A1 - Werner, K. A1 - Kruk, J. W. A1 - Hamann, Wolf-Rainer A1 - Sander, Andreas Alexander Christoph A1 - Todt, Helge Tobias T1 - The rapid evolution of the exciting star of the Stingray nebula JF - Astronomy and astrophysics : an international weekly journal N2 - Context. SAO 244567, the exciting star of the Stingray nebula, is rapidly evolving. Previous analyses suggested that it has heated up from an effective temperature of about 21 kK in 1971 to over 50 kK in the 1990s. Canonical post-asymptotic giant branch evolution suggests a relatively high mass while previous analyses indicate a low-mass star. Aims. A comprehensive model-atmosphere analysis of UV and optical spectra taken during 1988-2006 should reveal the detailed temporal evolution of its atmospheric parameters and provide explanations for the unusually fast evolution. Methods. Fitting line profiles from static and expanding non-LTE model atmospheres to the observed spectra allowed us to study the temporal change of effective temperature, surface gravity, mass-loss rate, and terminal wind velocity. In addition, we determined the chemical composition of the atmosphere. Results. We find that the central star has steadily increased its effective temperature from 38 kK in 1988 to a peak value of 60 kK in 2002. During the same time, the star was contracting, as concluded from an increase in surface gravity from log g = 4.8 to 6.0 and a drop in luminosity. Simultaneously, the mass-loss rate declined from log(M/M-circle dot yr(-1)) = -9.0 to -11.6 and the terminal wind velocity increased from v(infinity) = 1800 km s(-1) to 2800 km s(-1). Since around 2002, the star stopped heating and has cooled down again to 55 kK by 2006. It has a largely solar surface composition with the exception of slightly subsolar carbon, phosphorus, and sulfur. The results are discussed by considering different evolutionary scenarios. Conclusions. The position of SAO 244567 in the log T-eff-log g plane places the star in the region of sdO stars. By comparison with stellar-evolution calculations, we confirm that SAO 244567 must be a low-mass star (M < 0.55 M-circle dot). However, the slow evolution of the respective stellar evolutionary models is in strong contrast to the observed fast evolution and the young planetary nebula with a kinematical age of only about 1000 years. We speculate that the star could be a late He-shell flash object. Alternatively, it could be the outcome of close-binary evolution. Then SAD 244567 would be a low-mass (0.354 M-circle dot) helium pre-white dwarf after the common-envelope phase, during which the planetary nebula was ejected. KW - stars: abundances KW - stars: evolution KW - stars: AGB and post-AGB KW - stars: individual: SAO 244567 KW - stars: fundamental parameters KW - planetary nebulae: individual: Stingray nebula (Henize 3-1357) Y1 - 2014 U6 - https://doi.org/10.1051/0004-6361/201323189 SN - 0004-6361 SN - 1432-0746 VL - 565 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Steyrleuthner, Robert A1 - Di Pietro, Riccardo A1 - Collins, Brian A. A1 - Polzer, Frank A1 - Himmelberger, Scott A1 - Schubert, Marcel A1 - Chen, Zhihua A1 - Zhang, Shiming A1 - Salleo, Alberto A1 - Ade, Harald W. A1 - Facchetti, Antonio A1 - Neher, Dieter T1 - The Role of Regioregularity, Crystallinity, and Chain Orientation on Electron Transport in a High-Mobility n-Type Copolymer JF - Journal of the American Chemical Society Y1 - 2014 U6 - https://doi.org/10.1021/ja4118736 SN - 0002-7863 VL - 136 IS - 11 SP - 4245 EP - 4256 PB - American Chemical Society CY - Washington ER - TY - JOUR A1 - Schleussner, Carl-Friedrich A1 - Runge, Jakob A1 - Lehmann, Jasvcha A1 - Levermann, Anders T1 - The role of the North Atlantic overturning and deep ocean for multi-decadal global-mean-temperature variability JF - Earth system dynamics Y1 - 2014 U6 - https://doi.org/10.5194/esd-5-103-2014 SN - 2190-4979 SN - 2190-4987 VL - 5 IS - 1 SP - 103 EP - 115 PB - Copernicus CY - Göttingen 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 - Evans, T. M. A1 - Murphy, M. T. A1 - Whitmore, J. B. A1 - Misawa, T. A1 - Centurion, Martin A1 - Lopez, S. A1 - Martins, C. J. A. P. A1 - Molaro, P. A1 - Petitjean, P. A1 - Rahmani, H. A1 - Srianand, R. A1 - Wendt, Martin T1 - The UVES Large Program for testing fundamental physics - III. Constraints on the fine-structure constant from three telescopes JF - Monthly notices of the Royal Astronomical Society KW - intergalactic medium KW - quasars: absorption lines KW - quasars: individual: HS 1549+1919 KW - cosmology: miscellaneous KW - cosmology: observations Y1 - 2014 U6 - https://doi.org/10.1093/mnras/stu1754 SN - 0035-8711 SN - 1365-2966 VL - 445 IS - 1 SP - 128 EP - 150 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Sander, Andreas Alexander Christoph A1 - Todt, Helge Tobias A1 - Hainich, Rainer A1 - Hamann, Wolf-Rainer T1 - The Wolf-Rayet stars in M31 I. Analysis of the late-type WN stars JF - Astronomy and astrophysics : an international weekly journal N2 - Context. Comprehensive studies of Wolf-Rayet stars were performed in the past for the Galactic and the LMC population. The results revealed significant differences, but also unexpected similarities between the WR populations of these different galaxies. Analyzing the WR stars in M 31 will extend our understanding of these objects in different galactic environments. Aims. The present study aims at the late-type WN stars in M 31. The stellar and wind parameters will tell about the formation of WR stars in other galaxies with different metallicity and star formation histories. The obtained parameters will provide constraints to the evolution of massive stars in the environment of M 31. Methods. We used the latest version of the Potsdam Wolf-Rayet model atmosphere code to analyze the stars via fitting optical spectra and photometric data. To account for the relatively low temperatures of the late WN I 0 and WN I I subtypes, our WN models have been extended into this temperature regime. Results. Stellar and atmospheric parameters are derived for all known late-type WN stars in M 31 with available spectra. All of these stars still have hydrogen in their outer envelopes, some of them up to 50% by mass. The stars are located on the cool side of the zero age main sequence in the Hertzsprung-Russell diagram, while their luminosities range from 105 to 1064). It is remarkable that no star exceeds 106 L. Conclusions. If formed via single-star evolution, the late-type WN stars in M 31 stem from an initial mass range between 20 and 60 M-circle dot. From the very late-type WN9-11 stars, only one star is located in the S Doradus instability strip. We do not find any late-type WN stars with the high luminosities known in the Milky Way. KW - stars: massive KW - stars: evolution KW - stars: mass-loss KW - stars: Wolf-Rayet KW - stars: atmospheres KW - stars: winds KW - outflows Y1 - 2014 U6 - https://doi.org/10.1051/0004-6361/201323240 SN - 0004-6361 SN - 1432-0746 VL - 563 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Hainich, Rainer A1 - Ruehling, Ute A1 - Todt, Helge Tobias A1 - Oskinova, Lidia M. A1 - Liermann, A. A1 - Graefener, G. A1 - Foellmi, C. A1 - Schnurr, O. A1 - Hamann, Wolf-Rainer T1 - The Wolf-Rayet stars in the Large Magellanic Cloud - A comprehensive analysis of the WN class JF - Astronomy and astrophysics : an international weekly journal N2 - Context. Massive stars, although being important building blocks of galaxies, are still not fully understood. This especially holds true for Wolf-Rayet (WR) stars with their strong mass loss, whose spectral analysis requires adequate model atmospheres. Aims. Following our comprehensive studies of the WR stars in the Milky Way, we now present spectroscopic analyses of almost all known WN stars in the LMC. Methods. For the quantitative analysis of the wind-dominated emission-line spectra, we employ the Potsdam Wolf-Rayet (PoWR) model atmosphere code. By fitting synthetic spectra to the observed spectral energy distribution and the available spectra (ultraviolet and optical), we obtain the physical properties of 107 stars. Results. We present the fundamental stellar and wind parameters for an almost complete sample of WN stars in the LMC. Among those stars that are putatively single, two different groups can be clearly distinguished. While 12% of our sample are more luminous than 10(6) L-circle dot and contain a significant amount of hydrogen, 88% of the WN stars, with little or no hydrogen, populate the luminosity range between log (L/L-circle dot) = 5.3 ... 5.8. Conclusions. While the few extremely luminous stars (log (L/L-circle dot) > 6), if indeed single stars, descended directly from the main sequence at very high initial masses, the bulk of WN stars have gone through the red-supergiant phase. According to their luminosities in the range of log (L/L-circle dot) = 5.3 ... 5.8, these stars originate from initial masses between 20 and 40 M-circle dot. This mass range is similar to the one found in the Galaxy, i.e. the expected metallicity dependence of the evolution is not seen. Current stellar evolution tracks, even when accounting for rotationally induced mixing, still partly fail to reproduce the observed ranges of luminosities and initial masses. Moreover, stellar radii are generally larger and effective temperatures correspondingly lower than predicted from stellar evolution models, probably due to subphotospheric inflation. KW - stars: Wolf-Rayet KW - Magellanic Clouds KW - stars: early-type KW - stars: atmospheres KW - stars: winds, outflows KW - stars: mass-loss Y1 - 2014 U6 - https://doi.org/10.1051/0004-6361/201322696 SN - 0004-6361 SN - 1432-0746 VL - 565 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Rumyantsev, Artem M. A1 - Santer, Svetlana A1 - Kramarenko, Elena Yu. T1 - Theory of collapse and overcharging of a polyelectrolyte microgel induced by an oppositely charged surfactant JF - Macromolecules : a publication of the American Chemical Society N2 - We report on the theoretical study of interaction of ionic surfactants with oppositely charged microgel particles in dilute solutions. Two approaches are proposed. Within the first approach, the micellization of the surfactants inside the microgel is taken into account while the second model focuses on the hydrophobic interactions of the surfactant tails with the hydrophobic parts of microgel subchains. It has been shown that microgels effectively absorb surfactant ions. At low surfactant concentration this absorption is realized due to an ion exchange between microgel counterions and surfactant ions. The ion exchange is significantly affected by the amount of the microgel counterions initially trapped within the microgel particles which depends on the size of the microgel, its ionization degree, cross-linking density as well as polymer concentration in the solution. Increase of the surfactant concentration causes contraction of the microgels, which can be realized as either a continuous shrinking or a jump-like collapse transition depending on the system parameters. In the collapsed state additional absorption of surfactants by microgels takes place due to an energy gain from micellization or hydrophobic interactions. This leads to microgel precipitation and successive microgel overcharging at an excess of the surfactant in the solution. The theoretical results are compared with the existing experimental data, in particular, on photosensitive surfactant/microgel complexes. Y1 - 2014 U6 - https://doi.org/10.1021/ma500637d SN - 0024-9297 SN - 1520-5835 VL - 47 IS - 15 SP - 5388 EP - 5399 PB - American Chemical Society CY - Washington ER -