TY - JOUR A1 - Guliakova, A. A. A1 - Gorokhovatsky, Yu. A. A1 - Galikhanov, M. F. A1 - Frübing, Peter T1 - Thermoactivational spectroscopy of the high impact polystyrene based composite films T1 - Термоактивационная спектроскопия композитных полимерных пленок на основе ударопрочного полистирола JF - St. Petersburg Polytechnic University Journal : Physics and Mathematics N2 - The relaxation processes in the high impact polystyrene (HIPS) films filled with 2, 4, 6 vol.% of titanium dioxide (TiO2) of the rutile modification have been studied using the thermally stimulated depolarization current (TSDC) technique. Three relaxation processes were observed in the composite HIPS films. The first one (a-relaxation peak) appeared at about 93 degrees C and represented the glass transition. The second peak p was a high-temperature part of the first one and overlapped it. The p peak was caused by the release and subsequent motion of excess charges deposited during the electret preparation or the polarization process. The third peak appeared at about 150 degrees C and occurred only in the spectra of the composite films. The overlapping peaks were separated by the thermal cleaning technique. The subsequent application of the numerical methods (the Tikhonov regularization technique) allowed to determine the activation energy of the second process and to compare the obtained value with the corresponding data on the dielectric relaxation. N2 - С помощью метода токов термостимулированной деполяризации (ТСД) исследованы релаксационные процессы в пленках ударопрочного полистирола (УПС) без наполнителя и с различным содержанием диоксида титана TiO2 (2, 4, 6 об.%). На кривых тока ТСД, полученных для композитных пленок, обнаружено три пика. Первый (α-релаксация) возникает при температуре около 93 °C и соответствует переходу вещества из стеклообразного состояния в высокоэластическое. Второй (ρ-пик) появляется как высокотемпературное плечо α-пика и соответствует процессу высвобождения и движения избыточных носителей заряда. Наличие третьего пика при температуре около 150 ºС характерно только для композитных пленок УПС. Разделение перекрывающихся α- и ρ-пиков проведено методом частичной термоочистки. Последующее применение регуляризующих алгоритмов Тихонова позволило определить энергию активации второго процесcа и сравнить полученное значение с результатом, полученным методом диэлектрической спектроскопии. KW - thermoactivational spectroscopy KW - high impact polystyrene KW - titanium dioxide Y1 - 2019 U6 - https://doi.org/10.18721/JPM.12401 SN - 2405-7223 SN - 2618-8686 SN - 2304-9782 VL - 12 IS - 4 SP - 9 EP - 16 PB - Elsevier CY - Amsterdam ER - TY - JOUR A1 - Daute, Daniela T1 - Übermolekulare Strukturbildung durch Selbstorganisation neuer discoider Arylaminotriazine and assoziierter Alkoxybenzoate Y1 - 1995 ER - TY - THES A1 - Fischer, Jost T1 - Über Synchronisationsphänomene nichtlinearer akustischer Oszillatoren T1 - About synchronization phenomena of nonlinear acoustic oscillators N2 - In dieser Arbeit werden die Effekte der Synchronisation nichtlinearer, akustischer Oszillatoren am Beispiel zweier Orgelpfeifen untersucht. Aus vorhandenen, experimentellen Messdaten werden die typischen Merkmale der Synchronisation extrahiert und dargestellt. Es folgt eine detaillierte Analyse der Übergangsbereiche in das Synchronisationsplateau, der Phänomene während der Synchronisation, als auch das Austreten aus der Synchronisationsregion beider Orgelpfeifen, bei verschiedenen Kopplungsstärken. Die experimentellen Befunde werfen Fragestellungen nach der Kopplungsfunktion auf. Dazu wird die Tonentstehung in einer Orgelpfeife untersucht. Mit Hilfe von numerischen Simulationen der Tonentstehung wird der Frage nachgegangen, welche fluiddynamischen und aero-akustischen Ursachen die Tonentstehung in der Orgelpfeife hat und inwiefern sich die Mechanismen auf das Modell eines selbsterregten akustischen Oszillators abbilden lässt. Mit der Methode des Coarse Graining wird ein Modellansatz formuliert. N2 - In this study, synchronization properties observed in a system of nonlinear acoustic oscillators in form of two coupled organ pipes are investigated. From given measurements we extract the effects of synchronization one would expect typically. Furthermore we set our focus to the domains of transition into the synchronization region, when the system is complete synchronized and when it tears off, under the condition of different coupling strengths. We analyze and discuss the observed phenomena concerning their nonlinearities. Using numerical, fluid-dynamic and aeroacoustic simulation techniques we investigate how an organ pipe can be understand as a self-sustained, acoustic oscillator. With the results of the numerical simulations we show, how to reduce the complex fluid-dynamical interplay with the acoustic field inside the pipe to a self-sustained acoustic oscillator. For this process we use the coarse graining method. KW - Physik KW - Synchronisation KW - Orgelpfeife KW - nichtlinear KW - Akustik KW - physics KW - synchronization KW - organ pipe KW - nonlinear KW - acoustics Y1 - 2012 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-63618 ER - TY - THES A1 - Hertzsch, Jan-Martin T1 - Über nichtelastische Kollisionen und ihren Einfluß auf die Strukturbildung in planetaren Ringen Y1 - 1996 ER - TY - THES A1 - Rettig, Robert T1 - Über die Anisotropie der Kosmischen Strahlung Y1 - 2016 ER - TY - THES A1 - Schollmeyer, Hauke T1 - Zweidimensionale molekulare Ordnung und Strukturbildung : Triakontan an planaren SiO2/Luft-Grenzflächen Y1 - 2002 ER - TY - THES A1 - Liepertz, Sven Christian T1 - Zusammenhang zwischen dem Professionswissen von Physiklehrkräften, dem sachstrukturellen Angebot des Unterrichts und der Schülerleistung T2 - Studien zum Physik- und Chemielernen ; 224 Y1 - 2017 SN - 978-3-8325-4480-5 PB - Logos CY - Berlin ER - TY - JOUR A1 - Mikelskis, Helmut T1 - Zur Ökologisierung des Lernprozesses : Versuch über einen vernachlässigten Aspekt von Umweltbildung Y1 - 1993 SN - 3-89088-073-8 ER - TY - THES A1 - Pedzisz, Bozena T1 - Zur Rolle historischer Betrachtungen im Physikunterricht unter besonderer Berücksichtigung grundlegender Experimente Y1 - 1993 ER - TY - JOUR A1 - Starauschek, Erich T1 - Zur Rolle der Sprache beim Lernen von Physik Y1 - 2006 SN - 3-589-22148-8 ER - TY - THES A1 - Krey, Olaf T1 - Zur Rolle der Mathematik in der Physik : Wissenschaftstheoretische Aspekte und Vorstellungen Physiklernender T1 - The role of mathematics in physics : considerations from the philosophy of science and learners' conceptions N2 - Mathematik spielt im Physikunterricht eine nicht unerhebliche Rolle - wenn auch eine zwiespältige. Oft wird sie sogar zum Hindernis beim Lernen von Physik und kann ihr emanzipatorisches Potenzial nicht entfalten. Die vorliegende Arbeit stellt zwei Bausteine für eine begründete Konzeption zum Umgang mit Mathematik beim Lernen von Physik zur Verfügung. Im Theorieteil der Arbeit werden zum Einen wissenschaftstheoretische Aspekte der Rolle der Mathematik in der Physik aufgearbeitet und der physikdidaktischen Forschungsgemeinschaft im Zusammenhang zugänglich gemacht. Zum anderen werden Forschungsergebnisse zu Vorstellungen Lernender über Physik und Mathematik sowie im Bereich der Epistemologie zusammengestellt. Im empirischen Teil der Arbeit werden Vorstellungen zur Rolle der Mathematik in der Physik von Schülerinnen und Schülern der Klassenstufen 10 und 12 sowie Physik-Lehramtstudierenden im Grundstudium mit Hilfe eines Fragebogens erhoben und unter Verwendung inhaltsanalytischer bzw. statistischer Methoden ausgewertet. Die Ergebnisse zeigen unter Anderem, dass Mathematik im Physikunterricht entgegen gängiger Meinungen bei den Lernenden nicht negativ, aber zumindest bei jüngeren Lernenden formal und algorithmisch konnotiert ist. N2 - Mathematics plays an important, but ambivalent role in the physics classroom. Often mathematics becomes an obstacle in learning physics and cannot reveal its emancipatory potential. This thesis provides two components of a well-grounded conception for handling mathematics in the learning of physics. In the theoretical part of the thesis epistemological aspects of the role of mathematics in physics are being processed and made accessible to the community of physics education researchers. At the same time, research data on learners’ epistemological beliefs about physics and mathematics are compiled. In the empirical part of the thesis a questionnaire was designed to collect data on beliefs about the role of mathematics in physics from pupils of grade 10 and 12 as well as undergraduate physics teacher students. Content-analytical and statistical methods have been applied in the processing of the questionnaires. The results revealed, among others, that mathematics in the physics classroom is not, against common belief, evaluated negatively by learners. Yet, at least younger learners perceive the use of mathematics in physics to be mainly formal and algorithmic. KW - Physik KW - Wissenschaftstheorie KW - Vorstellungen KW - Mathematikdidaktik KW - Physikdidaktik KW - physics KW - philosophy of science KW - conceptions KW - mathematics education KW - science education Y1 - 2011 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-59412 ER - TY - THES A1 - Meister, Claudia-Veronika T1 - Zur physikalischen Theorie für Plasmen im Nichtgleichgewicht Y1 - 1995 ER - TY - THES A1 - Carroll, Thorsten Anthony T1 - Zur Linienentstehung und Diagnostik in kleinskaligen Magnetfeldern der solaren Photosphäre Y1 - 2004 ER - TY - JOUR A1 - Fruhner, Horst A1 - Czichocki, G. T1 - Zur Bestimmung der kritischen Mizellkonzentration (CMC) Y1 - 1996 ER - TY - THES A1 - Fortmann, Martin T1 - Zum Einfluß tropodhärischer Aerosole auf das Klima der Arktis Y1 - 2003 ER - TY - THES A1 - Gellert, Marcus T1 - Zum Dynamoeffekt in extern getriebenen Strömungen N2 - Die Frage nach der Herkunft und der dynamischen Entwicklung langlebiger kosmischer Magnetfelder ist in vielen Details noch unbeantwortet. Es besteht zwar kein Zweifel daran, dass das Magnetfeld der Erde und anderer kosmischer Objekte durch den sogenannten Dynamoeffekt verursacht werden, der genaue Mechanismus als auch die notwendigen Voraussetzungen und Randbedingungen der zugrundeliegenden Strömungen sind aber weitgehend unbekannt. Die für einen Dynamo interessanten Strömungsmuster, die im Inneren von Himmelskörpern durch Konvektion und differentielle Rotation entstehen, sind Konvektionsrollen parallel zur Rotationsachse. Auf einer Strömung mit eben solcher Geometrie, der sogenannten Roberts-Strömung, basieren die in der vorliegenden Arbeit untersuchten Dynamomodelle. Mit Methoden der nichtlinearen Dynamik wird versucht, das Systemverhalten bei Änderung der Systemparamter genauer zu charakterisieren. Die numerischen Untersuchungen beginnen mit einer Analyse der Dynamoaktivität der Roberts-Strömung in Abhängigkeit von den zwei freien Parametern in den Modellgleichungen, der magnetischen Prandtl-Zahl und der Stärke des Energieinputs. Gefunden werden verschiedene Lösungstypen die von einem stationären Magnetfeld über periodische bis zu chaotischen Zuständen reichen. Die yugrundeliegenden Symmetrien werden beschrieben und die Bifurkationen, die zum Wechsel der Lösungstypen führen, charakterisiert. Zusätzlich gibt es Bereiche bei sehr kleinen Prandtl-Zahlen, in denen überhaupt kein Dynamo existiert. Dieses Verhalten wird in der Literatur auch für viele andere numerisch ausgewertete Modelle beschrieben. Im Übergangsbereich zwischen dynamoaktivem und dynamoinaktivem Bereich wird das Auftreten einer sogenannten Blowout-Bifurkation gefunden. Desweiteren beschäftigt sich die Arbeit mit der Frage, inwiefern Helizität, also eine schraubenförmige Bewegung, der Strömung den Dynamoeffekt beeinflusst. Dazu werden ähnliche Strömungstypen verglichen, die sich hauptsächlich in ihrem Helizitätswert unterscheiden. Es wird gefunden, dass ein bestimmter Wert der Helizität nicht unterschritten werden darf, um einen stabilen Roberts-Dynamo zu erhalten. N2 - The question of origin and development of longlasting cosmic magnetic fields is in many details an unanswered question. There is no doubt that the magnetic fields of cosmic objects like the earth, the sun and larger structures are caused by the so called dynamo effect. The exact mechanism as well as the necassary properties and boundary conditions for the underlying flow field are mostly unknown. The flow pattern believed to act as the source of dynamo activity in the inner of cosmic bodies are convection-like rolls parallel to the rotation axis of this objects and are results of the acting body forces due to differential rotation and thermal convection. The basis of the considered dynamo model is a flow field revealing such flow structures, the so called Roberts flow. The numerical investigations start with an analysis of dynamo activity of the Roberts flow in dependence on the two free parameters magnetic Prandtl number and forcing strength. The model shows different types of solutions starting from steady magnetic states in a very small parameter region at larger magnetic Prandtl numbers, time-periodic solutions and chaotic behavior for stronger forcing. For small magnetic Prandtl numbers the system doesn't carry any magnetic field. This 'small Prandtl number problem' is in accordance with the behavior of several other numerically investigated dynamo models described in the literature. The transient region between dynamo activity and the non-magnetic states can be classified by a so-called blowout bifurcation. Furthermore the investigation deals with the question in what way the helical structure of the flow field indicated by a non-vanishing kinetic helicity influences the dynamo process. The comparison of very similar flow families, mainly distinguishable by their different helicity values, leads to the result that beneath a lower bound no stable Roberts dynamo is working. T2 - Zum Dynamoeffekt in extern getriebenen Strömungen KW - Dynamo KW - Dynamoeffekt KW - Magnetfelderzeugung KW - Roberts-Strömung KW - Helizität KW - dynamo KW - dynamo effect KW - magnetic field generation KW - Roberts flow KW - helicity Y1 - 2004 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-0001705 ER - TY - JOUR A1 - Mikelskis, Helmut T1 - Zukunftsperspektiven physikdidaktischer Forschung im vereinigten Deutschland Y1 - 1993 SN - 3-88064-223-0 ER - TY - JOUR A1 - Mikelskis, Helmut T1 - Zukunftsperspektiven der Bildung im Informationszeitalter und in der Wissensgesellschaft Y1 - 2001 ER - TY - JOUR A1 - Troll, Günter A1 - Beim Graben, Peter T1 - Zipfs law is not a consequence of the central limit theorem Y1 - 1998 ER - TY - JOUR A1 - Blasius, Bernd A1 - Toenjes, Ralf T1 - Zipf's Law in the popularity distribution of chess openings N2 - We perform a quantitative analysis of extensive chess databases and show that the frequencies of opening moves are distributed according to a power law with an exponent that increases linearly with the game depth, whereas the pooled distribution of all opening weights follows Zipf's law with universal exponent. We propose a simple stochastic process that is able to capture the observed playing statistics and show that the Zipf law arises from the self-similar nature of the game tree of chess. Thus, in the case of hierarchical fragmentation the scaling is truly universal and independent of a particular generating mechanism. Our findings are of relevance in general processes with composite decisions. Y1 - 2009 UR - http://prl.aps.org/ U6 - https://doi.org/10.1103/Physrevlett.103.218701 SN - 0031-9007 ER - TY - JOUR A1 - Lange, Ilja A1 - Reiter, Sina A1 - Kniepert, Juliane A1 - Piersimoni, Fortunato A1 - Paetzel, Michael A1 - Hildebrandt, Jana A1 - Brenner, Thomas J. K. A1 - Hecht, Stefan A1 - Neher, Dieter T1 - Zinc oxide modified with benzylphosphonic acids as transparent electrodes in regular and inverted organic solar cell structures JF - Applied physics letters N2 - An approach is presented to modify the work function of solution-processed sol-gel derived zinc oxide (ZnO) over an exceptionally wide range of more than 2.3 eV. This approach relies on the formation of dense and homogeneous self-assembled monolayers based on phosphonic acids with different dipole moments. This allows us to apply ZnO as charge selective bottom electrodes in either regular or inverted solar cell structures, using poly(3-hexylthiophene): phenyl-C71-butyric acid methyl ester as the active layer. These devices compete with or even surpass the performance of the reference on indium tin oxide/poly(3,4-ethylenedioxythiophene) polystyrene sulfonate. Our findings highlight the potential of properly modified ZnO as electron or hole extracting electrodes in hybrid optoelectronic devices. (C) 2015 AIP Publishing LLC. Y1 - 2015 U6 - https://doi.org/10.1063/1.4916182 SN - 0003-6951 SN - 1077-3118 VL - 106 IS - 11 PB - American Institute of Physics CY - Melville ER - TY - JOUR A1 - Rosenhahn, Axel A1 - Finlay, John A. A1 - Pettit, Michala E. A1 - Ward, Andy A1 - Wirges, Werner A1 - Gerhard, Reimund A1 - Callow, Maureen E. A1 - Grunze, Michael A1 - Callow, James A. T1 - Zeta potential of motile spores of the green alga Ulva linza and the influence of electrostatic interactions on spore settlement and adhesion strength N2 - The zeta potential of the motile spores of the green alga (seaweed) Ulva linza was quantified by video microscopy in combination with optical tweezers and determined to be -19.3ñ1.1 mV. The electrostatic component involved in the settlement and adhesion of spores was studied using electret surfaces consisting of PTFE and bearing different net charges. As the surface chemistry remains the same for differently charged surfaces, the experimental results isolate the influence of surface charge and thus electrostatic interactions. Ulva spores were demonstrated to have a reduced tendency to settle on negatively charged surfaces and when they did settle the adhesion strength of settled spores was lower than with neutral or positively charged surfaces. These observations can be ascribed to electrostatic interactions. Y1 - 2009 UR - http://biointerphases.org/ U6 - https://doi.org/10.1116/1.3110182 SN - 1559-4106 ER - TY - JOUR A1 - Mellinger, Axel A1 - Flores Suárez, Rosaura A1 - Singh, Rajeev A1 - Wegener, Michael A1 - Wirges, Werner A1 - Gerhard, Reimund T1 - Zerstörungsfreie Tomographie von Raumladungs- und Polarisationsverteilungen mittles Wärmepulsen N2 - Non-destructive, three-dimensional imaging of space-charge and polarization distributions in electret materials has been implemented by means of laser-induced thermal pulses. In pyroelectric films of poled poly(vinylidene fluoride), images of up to 45 x 45 pixels with a depth resolution of less than 0.5 mu m and a lateral resolution of 40 mu m were recorded, the latter being limited by fast thermal diffusion in the absorbing metallic front electrode. Initial applications include the analysis of polarization distributions in corona-poled piezoelectric sensor cables and the detection of patterned space-charge distributions in polytetrafluoroethylene films. Y1 - 2007 UR - http://www.oldenbourg-link.com/loi/teme U6 - https://doi.org/10.1524/teme.2007.74.9.437 SN - 0171-8096 ER - TY - BOOK A1 - Beta, Carsten T1 - Zelldynamik aus Sicht der Strukturbildung : physikalische Konzepte für ein biologisches Problem : Antrittsvorlesung 2008-06-05 N2 - Was lebt ist in Bewegung. Diese einfache Assoziation gilt nicht nur für ausgewachsene Organismen, sondern auch für einzelne Zellen, die kleinsten lebenden Bausteine der Natur. Die Beweglichkeit von Zellen spielt eine zentrale Rolle bei einer Vielzahl biologischer Vorgänge, wie zum Beispiel der Embryonalentwicklung, der Heilung von Wunden oder der krankhaften Ausbreitung von Krebszellen im Körper. Am Beispiel der Beweglichkeit einer einfachen Amöbe können grundlegende Mechanismen der Zelldynamik untersucht und auf der Grundlage physikalischer Konzepte erklärt werden. Y1 - 2008 UR - http://info.ub.uni-potsdam.de/multimedia/show_projekt.php?projekt_id=21 PB - Univ.-Bibl. CY - Potsdam ER - TY - THES A1 - Schwarz, Udo T1 - Zeitreihenanalyse astrophysikalischer Aktivitätsphänomene Y1 - 1994 ER - TY - THES A1 - Kopf, Markus T1 - Zeeman-Doppler Imaging of active late-type stars T1 - Zeeman-Doppler Imaging von späten aktiven Sternen N2 - Stellare Magnetfelder spielen eine wichtige Rolle bei der Entstehung und Entwicklung von Sternen. Leider entziehen sie sich aber, aufgrund ihrer großen Entfernung zur Erde, einer direkten Beobachtung. Dies gilt zumindest für derzeitige und in naher Zukunft zur Verfügung stehende Instrumente. Um aber beispielsweise zu verstehen, ob Magnetfelder durch einen Dynamoprozess generiert werden oder Überbleibsel der Sternentstehung sind, ist es zwingend erforderlich, die Oberflächenstruktur und die zeitliche Entwicklung von stellaren Feldern zu untersuchen. Glücklicherweise haben wir mit der Dopplerverschiebung sowie der Polarisation von Licht Mittel zur Verfügung, um indirekt die Magnetfeldtopologie entfernter Sternen zu rekonstruieren, wenn auch nur die schnell rotierender. Die auf den beiden genannten Effekten basierende Rekonstruktionsmethode ist unter dem Namen Zeeman-Doppler Imaging (ZDI) bekannt. Sie stellt eine leistungsfähige Methode dar, um aus rotationsverbreiterten Stokes Profilen schnell rotierender Sterne Oberflächenkartierungen der Temperatur und Magnetfeldverteilung zu erstellen. Durch das ZDI konnten in den vergangenen Jahren die Magnetfeldverteilungen zahlreicher Sterne rekonstruiert werden. Diese Methode stellt allerdings sehr hohe Anforderungen sowohl an die Instrumentierung als auch an die Rechenleistung und ist deshalb häufig mit zahlreichen Annahmen und Näherungen verbunden. Ziel dieser Arbeit war es, Methoden für ein ZDI zu entwickeln, das darauf ausgelegt ist, zeitaufgelöste spektropolarimetrische Daten von aktiven späten Sternen zu invertieren. Es sollte also insbesondere den komplexen und lokalen Magnetfeldstrukturen dieser Sterne Rechnung getragen werden. Um die Orientierung und Stärke solcher Felder zuverlässig rekonstruieren zu können, sollte die Inversion im Stande sein, alle vier Stokes-Komponenten einzubeziehen. Ferner war vorgesehen auf vollständigen polarisierten Strahlungstransportmodellierungen aufzubauen. Dies ermöglicht eine simultane und selbstkonsistente Temperatur- und Magnetfeld-Inversion, die damit dem komplexen Zusammenspiel zwischen Temperatur und Magnetfeld gerecht wird. Schließlich sollte die Anwendung eines neu zu entwickelnden ZDI Programms auf Stokes I und V Beobachtungen von II Pegasi (kurz: II Peg) erste Magnefeldkarten dieses sehr aktiven Sterns liefern. Um den hohen Rechenaufwand, der mit der Inversionsmethode einhergeht, besser bewältigen zu können, wurde zunächst eine schnelle Approximationsmethode für den polarisierten Strahlungstransport entwickelt. Sie basiert auf einer Hauptkomponentenanalyse (PCA) sowie auf künstlichen Neuronalen Netzen. Letztere approximieren den funktionalen Zusammenhang zwischen atmosphärischen Parametern und den zugehörigen lokalen Stokes Profilen. Inverse Probleme sind potentiell schlecht gestellt und erfordern in der Regel eine Regularisierung. Der entwickelte Ansatz verwendet eine lokale Entropie, die auf die Besonderheiten bei der Rekonstruktion lokalisierter Magnetfeder eingeht. Ein weiterer neuartiger Ansatz befasst sich mit der Rauschreduktion polarimetrischer Beobachtungsdaten. Er macht sich die Hauptkomponentenanalyse zu Nutze, um mit Hilfe einer Vielzahl beobachteter Spektrallinien, einzelne Linien mit drastisch vergrößertem Signal-zu-Rausch-Verhältnis wieder zu geben. Diese Methode hat gegenüber anderen Multi-Spektrallinien-Verfahren den Vorteil, nach wie vor eine Inversion auf der Basis einzelner Spektrallinien durchführen zu können. Schließlich wurde das Inversionsprogramm iMap entwickelt, das die zuvor genannten Methoden implementiert. Detaillierte Testrechnungen demonstrieren die Funktionsfähigkeit und Genauigkeit der schnellen Synthese-Methode und weisen einen Zeitgewinn von nahezu drei Größenordnungen gegenüber der konventionellen Strahlungstransportberechnung auf. Desweiteren untersuchen wir den Einfluss der verschiedenen Stokes Komponenten (IV bzw. IVQU) auf die Zuverlässigkeit, ein bekanntes Magnetfeld zu rekonstruieren. Damit belegen wir die Zuverlässigkeit unseres Inversionsprogrammes und zeigen darüber hinaus auch Einschränkungen von Magnetfeldinversionen im allgemeinen auf. Eine erste Inversion von Stokes I und V Profilen von II Peg liefert zum ersten Mal für diesen Stern simultan Temperatur- und Magnetfeldverteilungen. N2 - Stellar magnetic fields, as a crucial component of star formation and evolution, evade direct observation at least with current and near future instruments. However investigating whether magnetic fields are generated by a dynamo process or represent relics from the formation process, or whether they show a behavior similar to the sun or something very different, it is essential to investigate their structure and temporal evolution. Fortunately nature provides us with the possibility to indirectly observe surface topologies on distant stars by means of Doppler shift and polarization of light, though not without its challenges. Based on the mentioned effects, the so called Zeeman-Doppler Imaging technique is a powerful method to retrieve magnetic fields from rapid rotating stars based on measurements of spectropolarimetric observations in terms of Stokes profiles. In recent years, a large number of stellar magnetic field distributions could be reconstructed by Zeeman-Doppler Imaging (ZDI). However, the implementation of this method often relies on many approximations because, as an inversion method, it entails enormous computational requirements. The aim of this thesis is to develop methods for a ZDI, designed to invert time-resolved spectropolarimetric data of active late type stars, and to account for the expected complex and small scale magnetic fields on these stars. In order to reliably reconstruct the detailed field orientation and strength, the inversion method is employed to be able to use of all four Stokes components. Furthermore it is based on fully polarized radiative transfer calculations to account for the intricate interplay between temperature and magnetic field. Finally, the application of a newly developed ZDI code to Stokes I and V observations of II Pegasi (short: II Peg) was supposed to deliver the first magnetic surface maps for this highly active star. To accomplish the high computational burden of a radiative transfer based ZDI, we developed a novel approximation method to speed up the inversion process. It is based on Principal Component Analysis and Artificial Neural Networks. The latter approximate the functional mapping between atmospheric parameters and the corresponding local Stokes profiles. Inverse problems, as we are dealing with, are potentially ill-posed and require a regularization method. We propose a new regularization scheme, which implements a local entropy function that accounts for the peculiarities of the reconstruction of localized magnetic fields. To deal with the relatively large noise that is always present in polarimetric data, we developed a multi-line denoising technique based on Principal Component Analysis. In contrast to other multi-line techniques that extract from a large number of spectral lines a sort of mean profile, this method allows to extract individual spectral lines and thus allows for an inversion on the basis of specific lines. All these methods are incorporated in our newly developed ZDI code iMap, which is based on a conjugated gradient method. An in depth validation of our new synthesis method demonstrates the reliability and accuracy of this approach as well as a gain in computation time by almost three orders of magnitude relative to the conventional radiative transfer calculations. We investigated the influence of the different Stokes components (IV / IVQU) on the ability to reconstruct a known synthetic field configuration. In doing so we validate the capability of our inversion code, and we also assess limitations of magnetic field inversions in general. In a first application to II Peg, a K2 IV subgiant, we derived temperature and magnetic field surface distributions from spectropolarimetric data obtained in 2004 and 2007. It gives for the first time simultaneously the temporal evolution of the surface temperature and magnetic field distribution on II Peg. KW - Stellare Aktivität KW - Magnetfelder KW - Polarisation KW - Späte Sterne KW - Oberflächenstrukturen KW - stellar activity KW - magnetic fields KW - polarization KW - late-type stars KW - surface features Y1 - 2008 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-37387 ER - TY - JOUR A1 - Cioni, Maria-Rosa L. A1 - Bekki, Kenji A1 - Girardi, Leo A1 - de Grijs, Richard A1 - Irwin, Mike J. A1 - Ivanov, Valentin D. A1 - Marconi, Marcella A1 - Oliveira, Joana M. A1 - Piatti, Andres E. A1 - Ripepi, Vincenzo A1 - van Loon, Jacco Th. T1 - XVII. Proper motions of the Small Magellanic Cloud and the Milky Way globular cluster 47 Tucanae JF - Physical review : E, Statistical, nonlinear and soft matter physics N2 - Aims. In this study we use multi-epoch near-infrared observations from the VISTA survey of the Magellanic Cloud system (VMC) to measure the proper motions of different stellar populations in a tile of 1.5 deg2 in size in the direction of the Galactic globular cluster 47 Tuc. We obtain the proper motion of the cluster itself, of the Small Magellanic Cloud (SMC), and of the field Milky Way stars. Methods. Stars of the three main stellar components are selected according to their spatial distributions and their distributions in colour−magnitude diagrams. Their average coordinate displacement is computed from the difference between multiple Ks-band observations for stars as faint as Ks = 19 mag. Proper motions are derived from the slope of the best-fitting line among ten VMC epochs over a time baseline of ~1 yr. Background galaxies are used to calibrate the absolute astrometric reference frame. Results. The resulting absolute proper motion of 47 Tuc is (μαcos(δ), μδ) = (+7.26 ± 0.03, −1.25 ± 0.03) mas yr-1. This measurement refers to about 35 000 sources distributed between 10′ and 60′ from the cluster centre. For the SMC we obtain (μαcos(δ), μδ) = (+1.16 ± 0.07, −0.81 ± 0.07) mas yr-1 from about 5250 red clump and red giant branch stars. The absolute proper motion of the Milky Way population in the line of sight (l = 305.9, b = −44.9) of this VISTA tile is (μαcos(δ), μδ) = (+10.22 ± 0.14, −1.27 ± 0.12) mas yr-1 and has been calculated from about 4000 sources. Systematic uncertainties associated with the astrometric reference system are 0.18 mas yr-1. Thanks to the proper motion we detect 47 Tuc stars beyond its tidal radius. KW - proper motions KW - surveys KW - Magellanic Clouds KW - globular clusters: individual: 47 Tucanae Y1 - 2016 U6 - https://doi.org/10.1051/0004-6361/201527004 SN - 1432-0746 VL - 586 SP - 67 EP - 75 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Sanjurjo-Ferrrin, G. A1 - Torrejon, J. M. A1 - Postnov, K. A1 - Oskinova, Lida A1 - Rodes-Roca, J. J. A1 - Bernabeu, Guillermo T1 - XMM-Newton spectroscopy of the accreting magnetar candidate 4U0114+65 JF - Astronomy and astrophysics : an international weekly journal N2 - Methods. We analysed the energy-resolved light curve and the time-resolved X-ray spectra provided by the EPIC cameras on board XMM-Newton. We also analysed the first high-resolution spectrum of this source provided by the Reflection Grating Spectrometer. Results. An X-ray pulse of 9350 +/- 160 s was measured. Comparison with previous measurements confirms the secular spin up of this source. We successfully fit the pulse-phase-resolved spectra with Comptonisation models. These models imply a very small (r similar to 3 km) and hot (kT similar to 2-3 keV) emitting region and therefore point to a hot spot over the neutron star (NS) surface as the most reliable explanation for the X-ray pulse. The long NS spin period, the spin-up rate, and persistent X-ray emission can be explained within the theory of quasi-spherical settling accretion, which may indicate that the magnetic field is in the magnetar range. Thus, 4U0114+65 could be a wind-accreting magnetar. We also observed two episodes of low luminosity. The first was only observed in the low-energy light curve and can be explained as an absorption by a large over-dense structure in the wind of the B1 supergiant donor. The second episode, which was deeper and affected all energies, may be due to temporal cessation of accretion onto one magnetic pole caused by non-spherical matter capture from the structured stellar wind. The light curve displays two types of dips that are clearly seen during the high-flux intervals. The short dips, with durations of tens of seconds, are produced through absorption by wind clumps. The long dips, in turn, seem to be associated with the rarefied interclump medium. From the analysis of the X-ray spectra, we found evidence of emission lines in the X-ray photoionised wind of the B1Ia donor. The Fe K alpha line was found to be highly variable and much weaker than in other X-ray binaries with supergiant donors. The degree of wind clumping, measured through the covering fraction, was found to be much lower than in supergiant donor stars with earlier spectral types. Conclusions. The XMM-Newton spectroscopy provided further support for the magnetar nature of the neutron star in 4U0114+65. The light curve presents dips that can be associated with clumps and the interclump medium in the stellar wind of the mass donor. KW - X-rays: binaries KW - stars: winds, outflows KW - pulsars: individual: 4U0114+65 Y1 - 2017 U6 - https://doi.org/10.1051/0004-6361/201630119 SN - 1432-0746 VL - 606 SP - 4039 EP - 4042 PB - EDP Sciences CY - Les Ulis ER - TY - JOUR A1 - Ignace, Richard A1 - Oskinova, Lida A1 - Brown, John C. T1 - XMM-Newton Observations of the Nitrogen-Rich Wolf-Rayet star WR1 N2 - We present XMM-Newton results for the X-ray spectrum from the N-rich Wolf-Rayet (WR) star WR 1. The EPIC instrument was used to obtain a medium-resolution spectrum. The following features characterize this spectrum: (a) significant emission "bumps" appear that are coincident with the wavelengths of typical strong lines, such as Mg XI, Si XIII and S XV; (b) little emission is detected above 4 keV, in contrast to recent reports of a hard component in the stars WR 6 and WR 110 which are of similar subtype; and (c) evidence for sulfur K-edge absorption at about 2.6 keV, which could only arise from absorption of X-rays by the ambient stellar wind. The lack of hard emission in our dataset is suggestive that WR 1 may truly be a single star, thus representing the first detailed X-ray spectrum that isolates the WR wind alone (in contrast to colliding wind zones). Although the properties of the S-edge are not well-constrained by our data, it does appear to be real, and its detection indicates that at least some of the hot gas in WR 1 must reside interior to the radius of optical depth unity for the total absorptive opacity at the energy of the edge. Y1 - 2003 ER - TY - JOUR A1 - Sidoli, Lara A1 - Sguera, Vito A1 - Esposito, Paolo A1 - Oskinova, Lida A1 - Polletta, Maria del Carmen T1 - XMM-Newton discovery of very high obscuration in the candidate Supergiant Fast X-ray Transient AX J1714.1-3912 JF - Monthly notices of the Royal Astronomical Society N2 - We have analysed an archival XMM-Newton EPIC observation that serendipitously covered the sky position of a variable X-ray source AX J1714.1-3912, previously suggested to be a Supergiant Fast X-ray Transient (SFXT). During the XMM-Newton observation the source is variable on a timescale of hundred seconds and shows two luminosity states, with a flaring activity followed by unflared emission, with a variability amplitude of a factor of about 50. We have discovered an intense iron emission line with a centroid energy of 6.4 keV in the power law-like spectrum, modified by a large absorption (N-H similar to 10(24) cm(-2)), never observed before from this source. This X-ray spectrum is unusual for an SFXT, but resembles the so-called 'highly obscured sources', high mass X-ray binaries (HMXBs) hosting an evolved B[e] supergiant companion (sgB[e]). This might suggest that AX J1714.1-3912 is a new member of this rare type of HMXBs, which includes IGR J16318-4848 and CI Camelopardalis. Increasing this small population of sources would be remarkable, as they represent an interesting short transition evolutionary stage in the evolution of massive binaries. Nevertheless, AX J1714.1-3912 appears to share X-ray properties of both kinds of HMXBs (SFXT versus sgB[e] HMXB). Therefore, further investigations of the companion star are needed to disentangle the two hypothesis. KW - X-rays: binaries KW - X-rays: individual: AX J1714.1-3912 Y1 - 2022 U6 - https://doi.org/10.1093/mnras/stac691 SN - 0035-8711 SN - 1365-2966 VL - 512 IS - 2 SP - 2929 EP - 2935 PB - Oxford Univ. Press CY - Oxford ER - TY - CHAP A1 - Oskinova, Lida A1 - Hamann, Wolf-Rainer A1 - Feldmeier, Achim T1 - X-raying clumped stellar winds N2 - X-ray spectroscopy is a sensitive probe of stellar winds. X-rays originate from optically thin shock-heated plasma deep inside the wind and propagate outwards throughout absorbing cool material. Recent analyses of the line ratios from He-like ions in the X-ray spectra of O-stars highlighted problems with this general paradigm: the measured line ratios of highest ions are consistent with the location of the hottest X-ray emitting plasma very close to the base of the wind, perhaps indicating the presence of a corona, while measurements from lower ions conform with the wind-embedded shock model. Generally, to correctly model the emerging Xray spectra, a detailed knowledge of the cool wind opacities based on stellar atmosphere models is prerequisite. A nearly grey stellar wind opacity for the X-rays is deduced from the analyses of high-resolution X-ray spectra. This indicates that the stellar winds are strongly clumped. Furthermore, the nearly symmetric shape of X-ray emission line profiles can be explained if the wind clumps are radially compressed. In massive binaries the orbital variations of X-ray emission allow to probe the opacity of the stellar wind; results support the picture of strong wind clumping. In high-mass X-ray binaries, the stochastic X-ray variability and the extend of the stellar-wind part photoionized by X-rays provide further strong evidence that stellar winds consist of dense clumps. Y1 - 2007 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus-18133 ER - TY - THES A1 - Foster, Mary Grace T1 - X-Ray studies of exoplanet systems N2 - X-rays are integral to furthering our knowledge of exoplanetary systems. In this work we discuss the use of X-ray observations to understand star-planet interac- tions, mass-loss rates of an exoplanet’s atmosphere and the study of an exoplanet’s atmospheric components using future X-ray spectroscopy. The low-mass star GJ 1151 was reported to display variable low-frequency radio emission, which is an indication of coronal star-planet interactions with an unseen exoplanet. In chapter 5 we report the first X-ray detection of GJ 1151’s corona based on XMM-Newton data. Averaged over the observation, we detect the star with a low coronal temperature of 1.6 MK and an X-ray luminosity of LX = 5.5 × 1026 erg/s. This is compatible with the coronal assumptions for a sub-Alfvénic star- planet interaction origin of the observed radio signals from this star. In chapter 6, we aim to characterise the high-energy environment of known ex- oplanets and estimate their mass-loss rates. This work is based on the soft X-ray instrument on board the Spectrum Roentgen Gamma (SRG) mission, eROSITA, along with archival data from ROSAT, XMM-Newton, and Chandra. We use these four X-ray source catalogues to derive X-ray luminosities of exoplanet host stars in the 0.2-2 keV energy band. A catalogue of the mass-loss rates of 287 exoplan- ets is presented, with 96 of these planets characterised for the first time using new eROSITA detections. Of these first time detections, 14 are of transiting exoplanets that undergo irradiation from their host stars that is of a level known to cause ob- servable evaporation signals in other systems, making them suitable for follow-up observations. In the next generation of space observatories, X-ray transmission spectroscopy of an exoplanet’s atmosphere will be possible, allowing for a detailed look into the atmospheric composition of these planets. In chapter 7, we model sample spectra using a toy model of an exoplanetary atmosphere to predict what exoplanet transit observations with future X-ray missions such as Athena will look like. We then estimate the observable X-ray transmission spectrum for a typical Hot Jupiter-type exoplanet, giving us insights into the advances in X-ray observations of exoplanets in the decades to come. N2 - Röntgenstrahlen sind ein wesentlicher Bestandteil, um unser Wissen über extrasolare Planetensysteme zu vertiefen und zu erweitern. In dieser Arbeit erörtern wir den Einsatz von Röntgenbeobachtungen zum Verständnis von Stern-Planeten-Interaktionen, der Abschätzung von Massenverlustraten von Exoplanetenatmosphären und die Untersuchung der atmosphärischen Komponenten eines Exoplaneten mithilfe zukünftiger Röntgenspektroskopie. Beobachtungen des massearmen Sterns GJ 1151 deuten auf eine variable Emission niederfrequenter Radiostrahlung hin, was als Indiz für koronale Stern-Planeten-Wechselwirkungen mit einem unsichtbaren Exoplaneten angesehen wird. In Kapitel 5 berichten wir über den ersten Röntgennachweis der Korona von GJ 1151, basierend auf XMM-Newton Daten. Über die gesamte Beobachtungsdauer gemittelt, weisen wir den Stern mit einer niedrigen koronalen Temperatur von 1,6 MK und einer Röntgenluminosität von LX = 5, 5 ◊ 1026 erg/s nach. Dieser Nachweis im Röntgenlicht ist kompatibel mit der Annahme, dass sub-Alfvénische Wechselwirkungen zwischen stellarer Corona und Exoplanet die Ursache für die beobachteten Radiosignale des Sterns sind. Kapitel 6 zielt darauf ab, die hochenergetische Umgebung bekannter Exoplaneten zu charakterisieren und die Massenverlustraten der Planetenatmosphären abzuschätzen. Diese Arbeit basiert auf neu gewonnenen Daten des Instruments für weiche Röntgenstrahlung an Bord der Spectrum Roentgen Gamma (SRG) Mission, eROSITA, und wird komplementiert von Archivdaten von ROSAT, XMM-Newton und Chandra. Mithilfe dieser vier Röntgenquellenkataloge vermessen wir die Röntgenhelligkeit der Zentralsterne von bekannten Exoplanetensytemen im Energiebereich von 0,2-2 keV. Die Ergebnisse sind zusammen mit den errechneten Massenverlustraten von 287 Exoplaneten in einem Katalog zusammengefasst, darunter 96 Planeten, die zum ersten Mal durch neue eROSITA-Nachweise charakterisiert wurden. Bei 14 dieser Erstnachweise handelt es sich um transitierende Exoplaneten, die von ihrem Heimatstern so stark bestrahlt werden, dass beobachtbare Signale, ausgelöst durch die Verdampfung ihrer Atmosphäre, zu erwarten sind. Speziell diese Systeme eignen sich besonders für Folgebeobachtungen. Mit der nächsten Generation von Weltraumobservatorien wird die Röntgentransmissionsspektroskopie von extrasolaren Planetenatmosphären möglich sein, was nie dagewesene Details über die atmosphärische Zusammensetzung dieser Planeten ans Licht bringen wird. In Kapitel 7 modellieren wir Transmissionsspektren mithilfe eines vereinfachten Modells einer Exoplanetenatmosphäre um vorherzusagen, wie Transitbeobachtungen von Exoplaneten mit zukünftigen Röntgenmissionen wie Athena aussehen werden. Wir schätzen dann das beobachtbare Röntgentransmissionsspektrum für einen typischen Exoplaneten vom Typ Hot Jupiter ab, was uns einen Einblick in die zu erwartenden Fortschritte bei der Röntgenbeobachtung von Exoplaneten in den kommenden Jahrzehnten gibt. KW - exoplanets KW - x-rays KW - stellar physics KW - Exoplaneten KW - Röntgenstrahlen KW - stellare Physik Y1 - 2022 U6 - http://nbn-resolving.de/urn/resolver.pl?urn:nbn:de:kobv:517-opus4-562152 PB - xiii, 92 ER - TY - JOUR A1 - Reiche, Jürgen A1 - Barberka, Thomas Andreas A1 - Janietz, Dietmar A1 - Hofmann, Dieter A1 - Pietsch, Ullrich A1 - Brehmer, Ludwig T1 - X-ray structure investigation and computer modelling of Langmuir-Blodgett films formed from disc-shaped pentaalkines Y1 - 1994 ER - TY - JOUR A1 - Miedema, P. S. A1 - Mitzner, Rolf A1 - Ganschow, S. A1 - Föhlisch, Alexander A1 - Beye, Martin T1 - X-ray spectroscopy on the active ion in laser crystals JF - Physical chemistry, chemical physics : a journal of European Chemical Societies N2 - The active ions in typical laser crystals were studied with Resonant Inelastic X-ray Scattering (RIXS) and Partial Fluorescence Yield X-ray Absorption (PFY-XAS) spectroscopies as solid state model systems for dilute active centers. We analyzed Ti3+ and Cr3+ in alpha-Al2O3:Ti3+ and LiCaAlF6:Cr3+, respectively. The comparison of experimental data with semi-empirical multiplet calculations provides insights into the electronic structure and shows how measured crystal field energies are related across different spectroscopies. Y1 - 2017 U6 - https://doi.org/10.1039/c7cp03026f SN - 1463-9076 SN - 1463-9084 VL - 19 SP - 21800 EP - 21806 PB - Royal Society of Chemistry CY - Cambridge ER - TY - JOUR A1 - Pietsch, Ullrich A1 - Barberka, Thomas Andreas A1 - Geue, Thomas A1 - Stömmer, Ralph T1 - X-ray scattering from thin organic films and multilayers Y1 - 1997 ER - TY - THES A1 - Stömmer, Ralph T1 - X-ray scattering from silicon surfaces and thin oxides on silicon substrates Y1 - 1998 ER - TY - JOUR A1 - Stömmer, Ralph A1 - Göbel, H. A1 - Hub, W. A1 - Pietsch, Ullrich T1 - X-ray scattering from silicon surfaces Y1 - 1998 ER - TY - THES A1 - Baumbach, Tilo T1 - X-Ray scattering by periodic nanostructures Y1 - 2000 ER - TY - JOUR A1 - Pietsch, Ullrich A1 - Tsirelson, Vladimir G. A1 - Gorfan, S. V. T1 - X-ray scattering amplitude of an atom in a permanent external electric field Y1 - 2003 ER - TY - JOUR A1 - Pietsch, Ullrich A1 - Kubowicz, Stephan A1 - Thünemann, Andreas F. A1 - Geue, Thomas A1 - Watson, M. D. A1 - Tchebotareva, N. A1 - Müllen, K. T1 - X-ray reflectivity study of an amphiphilic hex-peri-hexabenzocoronene at a structured silicon wafer surface Y1 - 2003 ER - TY - JOUR A1 - Geue, Thomas A1 - Henneberg, Oliver A1 - Pietsch, Ullrich T1 - X-ray reflectivity from sinusoidal surface relief gratings Y1 - 2002 SN - 0023-4753 ER - TY - JOUR A1 - Pietsch, Ullrich T1 - X-ray reflectivity from sinusoidal surface relief gratings Y1 - 2002 ER - TY - JOUR A1 - Poloucek, P. A1 - Pietsch, Ullrich A1 - Geue, Thomas A1 - Symietz, Christian A1 - Brezesinski, Gerald T1 - X-ray reflectivity analysis of thin complex Langmuir-Blodgett films Y1 - 2001 ER - TY - JOUR A1 - Giewekemeyer, K. A1 - Krueger, S. P. A1 - Kalbfleisch, S. A1 - Bartels, Meike A1 - Beta, Carsten A1 - Salditt, T. T1 - X-ray propagation microscopy of biological cells using waveguides as a quasipoint source JF - Physical review : A, Atomic, molecular, and optical physics N2 - We have used x-ray waveguides as highly confining optical elements for nanoscale imaging of unstained biological cells using the simple geometry of in-line holography. The well-known twin-image problem is effectively circumvented by a simple and fast iterative reconstruction. The algorithm which combines elements of the classical Gerchberg-Saxton scheme and the hybrid-input-output algorithm is optimized for phase-contrast samples, well-justified for imaging of cells at multi-keV photon energies. The experimental scheme allows for a quantitative phase reconstruction from a single holographic image without detailed knowledge of the complex illumination function incident on the sample, as demonstrated for freeze-dried cells of the eukaryotic amoeba Dictyostelium discoideum. The accessible resolution range is explored by simulations, indicating that resolutions on the order of 20 nm are within reach applying illumination times on the order of minutes at present synchrotron sources. Y1 - 2011 U6 - https://doi.org/10.1103/PhysRevA.83.023804 SN - 1050-2947 VL - 83 IS - 2 PB - American Physical Society CY - College Park ER - TY - JOUR A1 - Toala, Jesús Alberto A1 - Oskinova, Lida A1 - Gonzalez-Galan, Ana A1 - Guerrero, Martín A. A1 - Ignace, R. A1 - Pohl, Martin T1 - X-RAY OBSERVATIONS OF BOW SHOCKS AROUND RUNAWAY O STARS. THE CASE OF zeta OPH AND BD+43 degrees 3654 JF - The astrophysical journal : an international review of spectroscopy and astronomical physics N2 - Non-thermal radiation has been predicted within bow shocks around runaway stars by recent theoretical works. We present X-ray observations toward the runaway stars zeta Oph by Chandra and Suzaku and of BD+43 degrees 3654 by XMM-Newton to search for the presence of non-thermal X-ray emission. We found no evidence of non-thermal emission spatially coincident with the bow shocks; nonetheless, diffuse emission was detected in the vicinity of zeta Oph. After a careful analysis of its spectral characteristics, we conclude that this emission has a thermal nature with a plasma temperature of T approximate to 2 x 10(6) K. The cometary shape of this emission seems to be in line with recent predictions of radiation-hydrodynamic models of runaway stars. The case of BD+43 degrees 3654 is puzzling, as non-thermal emission has been reported in a previous work for this source. KW - stars: individual (zeta Oph, BD+43 degrees 3654) KW - stars: winds, outflows Y1 - 2016 U6 - https://doi.org/10.3847/0004-637X/821/2/79 SN - 0004-637X SN - 1538-4357 VL - 821 PB - IOP Publ. Ltd. CY - Bristol ER - TY - JOUR A1 - Oskinova, Lida A1 - Feldmeier, Achim A1 - Hamann, Wolf-Rainer T1 - X-ray line profiles from structured stellar winds N2 - Absorbing material compressed in a number of thin shells is effectively less opaque for X-rays than smoothly distributed gas. The calculated X-ray emission line profiles are red-shifted if the emission arises from the starward side of the shells. Y1 - 2003 SN - 1-58381-133-8 ER - TY - JOUR A1 - Feldmeier, Achim A1 - Oskinova, Lida A1 - Hamann, Wolf-Rainer T1 - X-ray line emission from a fragmented stellar wind N2 - We discuss X-ray line formation in dense O star winds. A random distribution of wind shocks is assumed to emit X-rays that are partially absorbed by cooler wind gas. The cool gas resides in highly compressed fragments oriented perpendicular to the radial flow direction. For fully opaque fragments, we find that the blueshifted part of X-ray line profiles remains flat-topped even after severe wind attenuation, whereas the red part shows a steep decline. These box- type, blueshifted profiles resemble recent Chandra observations of the O3 star zeta Pup. For partially transparent fragments, the emission lines become similar to those from a homogeneous wind. Y1 - 2003 ER - TY - JOUR A1 - Poppenhäger, Katja A1 - Ketzer, Laura A1 - Mallonn, Matthias T1 - X-ray irradiation and evaporation of the four young planets around V1298 Tau JF - Monthly notices of the Royal Astronomical Society N2 - Planets around young stars are thought to undergo atmospheric evaporation due to the high magnetic activity of the host stars. Here we report on X-ray observations of V1298 Tau, a young star with four transiting exoplanets. We use X-ray observations of the host star with Chandra and ROSAT to measure the current high-energy irradiation level of the planets and employ a model for the stellar activity evolution together with exoplanetary mass-loss to estimate the possible evolution of the planets. We find that V1298 Tau is X-ray bright with log L-X [erg s(-1)] = 30.1 and has a mean coronal temperature of approximate to 9 MK. This places the star amongst the more X-ray luminous ones at this stellar age. We estimate the radiation-driven mass-loss of the exoplanets and find that it depends sensitively on the possible evolutionary spin-down tracks of the star as well as on the current planetary densities. Assuming the planets are of low density due to their youth, we find that the innermost two planets can lose significant parts of their gaseous envelopes and could be evaporated down to their rocky cores depending on the stellar spin evolution. However, if the planets are heavier and follow the mass-radius relation of older planets, then even in the highest XUV irradiation scenario none of the planets is expected to cross the radius gap into the rocky regime until the system reaches an age of 5 Gyr. KW - planets and satellites: atmospheres KW - planet-star interactions KW - stars: activity KW - stars: individual: V1298 Tau KW - X-rays: stars Y1 - 2020 U6 - https://doi.org/10.1093/mnras/staa1462 SN - 0035-8711 SN - 1365-2966 VL - 500 IS - 4 SP - 4560 EP - 4572 PB - Oxford Univ. Press CY - Oxford ER - TY - JOUR A1 - Geue, Thomas A1 - Schultz, Michael A1 - Grenzer, Jörg A1 - Natansohn, Almeria A1 - Rochon, Paul T1 - X-ray investigations of the molecular mobility with polymer surface gratings Y1 - 2000 ER - TY - JOUR A1 - Pietsch, Ullrich A1 - Geue, Thomas A1 - Henneberg, Oliver A1 - Saphiannikova, Marina T1 - X-ray investigations of formation efficiency of buried azobenzene polymer density gratings Y1 - 2003 UR - http://scitation.aip.org/journals/doc/JAPIAU-ft/vol_93/iss_6/3161_1.html U6 - https://doi.org/10.1063/1.1554753 ER -