@inproceedings{OPUS4-1658,
  title     = {Seelisch gesund von Anfang an : Programm und Abstracts des 26. Symposiums der Fachgruppe Klinische Psychologie und Psychotherapie der Deutschen Gesellschaft f{\"u}r Psychologie, 1. - 3. Mai 2008 in Potsdam},
  editor    = {Warschburger, Petra and Ihle, Wolfgang and Esser, G{\"u}nter},
  publisher = {Universit{\"a}tsverlag Potsdam},
  address   = {Potsdam},
  isbn      = {978-3-940793-34-8},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17551},
  pages     = {302},
  year      = {2008},
  abstract  = {Der Tagungsband enth{\"a}lt das Programm und die Abstracts des 26. Symposiums der Fachgruppe Klinische Psychologie und Psychotherapie der Deutschen Gesellschaft f{\"u}r Psychologie, veranstaltet an der Universit{\"a}t Potsdam vom 1. bis 3. Mai 2008. Etwa 450 Kongressteilnehmer pr{\"a}sentieren den aktuellen Forschungs- und Wissensstand der Klinischen Psychologie und Psychotherapie in Deutschland. Grußworte halten die brandenburgische Ministerin f{\"u}r Arbeit, Soziales, Gesundheit und Familie, Dagmar Ziegler, die Pr{\"a}sidentin der Universit{\"a}t Potsdam, Prof. Dr.-Ing. Dr. Sabine Kunst, sowie Prof. Dr. Michael Linden als Vertreter der Deutschen Gesellschaft f{\"u}r Psychiatrie, Psychotherapie und Nervenheilkunde (DGPPN). Zu den Themenschwerpunkten des Kongresses geh{\"o}ren Einflussfaktoren auf die psychische Gesundheit {\"A}lterer, Impulsivit{\"a}t, Schlaf- und Traumforschung in der Klinischen Psychologie, Behandlung von Essst{\"o}rungen, Wirksamkeitsstudien psychischer St{\"o}rungen des Kindes- und Jugendalters, Angst und Depression, Behandlung von Kriegs- und Folteropfern, Risiko- und Schutzfaktoren der Kindesentwicklung sowie Adipositas im Kindes- und Jugendalter. Außer den Vortr{\"a}gen gibt es eine Pr{\"a}sentation von etwa 150 Postern. Zum Programm der Tagung geh{\"o}rt ebenso die Verleihung des Klaus-Grawe-Awards for the Advancement of Innovative Research in Clinical Psychology and Psychotherapy an Prof. Dr. Timothy J. Strauman von der Duke University (USA), die Verleihung der Nachwuchswissenschaftler- und Posterpreise sowie ein Pre-conference Workshop f{\"u}r Doktorandinnen und Doktoranden der Klinischen Psychologie zum Thema "Verhaltens- und Molekulargenetik".},
  subject      = {Konferenz},
  language  = {de}
}
@inproceedings{Reimer2007,
  author    = {Reimer, A.},
  title     = {Clumping effects on non-thermal particle spectra in massive star systems},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18246},
  year      = {2007},
  abstract  = {Observational evidence exists that winds of massive stars are clumped. Many massive star systems are known as non-thermal particle production sites, as indicated by their synchrotron emission in the radio band. As a consequence they are also considered as candidate sites for non-thermal high-energy photon production up to gamma-ray energies. The present work considers the effects of wind clumpiness expected on the emitting relativistic particle spectrum in colliding wind systems, built up from the pool of thermal wind particles through diffusive particle acceleration, and taking into account inverse Compton and synchrotron losses. In comparison to a homogeneous wind, a clumpy wind causes flux variations of the emitting particle spectrum when the clump enters the wind collision region. It is found that the spectral features associated with this variability moves temporally from low to high energy bands with the time shift between any two spectral bands being dependent on clump size, filling factor, and the energy-dependence of particle energy gains and losses.},
  language  = {en}
}
@inproceedings{Weis2007,
  author    = {Weis, K.},
  title     = {Wind relics : clumps, inhomogeneities and outflows in LBV nebulae},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18235},
  year      = {2007},
  abstract  = {The most massive stars are those with the shortest but most active life. One group of massive stars, the Luminous Blue Variables (LBVs), of which only a few objects are known, are in particular of interest concerning the stability of stars. They have a high mass loss rate and are close to being instable. This is even more likely as rotation becomes an important factor in stellar evolution of these stars. Through massive stellar winds and sometimes giant eruptions, LBV nebulae are formed. Various aspects in the evolution in the LBV phase lead, beside the large scale morphological and kinematical differences, to a diversity of small structures like clumps, rims, and outflows in these nebulae.},
  language  = {en}
}
@inproceedings{RomeroOwockiAraudoetal.2007,
  author    = {Romero, G. E. and Owocki, S. P. and Araudo, A. T. and Townsend, R. H. D. and Benaglia, P.},
  title     = {Using gamma-rays to probe the clumped structure of stellar winds},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18210},
  year      = {2007},
  abstract  = {Gamma-rays can be produced by the interaction of a relativistic jet and the matter of the stellar wind in the subclass of massive X-ray binaries known as "microquasars". The relativistic jet is ejected from the surroundings of the compact object and interacts with cold protons from the stellar wind, producing pions that then quickly decay into gamma-rays. Since the resulting gamma-ray emissivity depends on the target density, the detection of rapid variability in microquasars with GLAST and the new generation of Cherenkov imaging arrays could be used to probe the clumped structure of the stellar wind. In particular, we show here that the relative fluctuation in gamma rays may scale with the square root of the ratio of porosity length to binary separation, \$\sqrt{h/a}\$, implying for example a ca. 10\% variation in gamma ray emission for a quite moderate porosity, h/a ∼ 0.01.},
  language  = {en}
}
@inproceedings{Nielsen2007,
  author    = {Nielsen, K. E.},
  title     = {On irregular line profiles in the optical spectrum of Eta Carinae},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18227},
  year      = {2007},
  abstract  = {The optical spectrum of Eta Carinae (η Car) is prominent in H I, He i and Fe ii wind lines, all of which vary both in absorption and emission with phase. The phase dependance is a consequence of the interaction between the two objects in the η Car binary (η Car A \& B). The binary system is enshrouded by ejecta from previous mass ejection events and consequently, η Car B is not directly observable. We have traced the He i lines over η Car's spectroscopic period, using HST/STIS data obtained with medium spectral, but high angular, resolving power, and created a radial velocity curve for the system. The He I lines are formed in the core of the system, and appear to be a composite of multiple features formed in spatially separated regions. The sources of their irregular line profiles are still not fully understood, but can be attributed to emission/absorption near the wind-wind interface and/or a direct consequence of the η Car A's, massive, clumpy wind. This paper will discuss the spectral variability, the narrow emission structure of the He i lines and how clumpiness of the winds may impede the construction of the reliable radial velocity curve, necessary for characterizations of especially η Car B.},
  language  = {en}
}
@inproceedings{Gull2007,
  author    = {Gull, T. R.},
  title     = {Eta Carinae viewed from different vantages},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18200},
  year      = {2007},
  abstract  = {The spatially-resolved winds of the massive binary, Eta Carinae, extend an arcsecond on the sky, well beyond the 10 to 20 milliarcsecond binary orbital dimension. Stellar wind line profiles, observed at very different angular resolutions of VLTI/AMBER, HST/STIS and VLT/UVES, provide spatial information on the extended wind interaction structure as it changes with orbital phase. These same wind lines, observable in the starlight scattered off the foreground lobe of the dusty Homunculus, provide time-variant line profiles viewed from significantly different angles. Comparisons of direct and scattered wind profiles observed in the same epoch and at different orbital phases provide insight on the extended wind structure and promise the potential for three-dimensional imaging of the outer wind structures. Massive, long-lasting clumps, including the nebularWeigelt blobs, originated during the two historical ejection events. Wind interactions with these clumps are quite noticeable in spatially-resolved spectroscopy. As the 2009.0 minimum approaches, analysis of existing spectra and 3-D modeling are providing bases for key observations to gain further understanding of this complex massive binary.},
  language  = {en}
}
@inproceedings{Cassinelli2007,
  author    = {Cassinelli, Joseph P.},
  title     = {Discussion: Magnetic fields, variability},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18195},
  year      = {2007},
  language  = {en}
}
@inproceedings{ReimerAharonianHintonetal.2007,
  author    = {Reimer, O. and Aharonian, Felix A. and Hinton, J. and Hofmann, W. and Hoppe, S. and Raue, M. and Reimer, A.},
  title     = {VHE gamma-rays from Westerlund 2 and implications for the inferred energetics},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18172},
  year      = {2007},
  abstract  = {The H.E.S.S. collaboration recently reported the discovery of VHE γ-ray emission coincident with the young stellar cluster Westerlund 2. This system is known to host a population of hot, massive stars, and, most particularly, the WR binary WR 20a. Particle acceleration to TeV energies in Westerlund 2 can be accomplished in several alternative scenarios, therefore we only discuss energetic constraints based on the total available kinetic energy in the system, the actual mass loss rates of respective cluster members, and implied gamma-ray production from processes such as inverse Compton scattering or neutral pion decay. From the inferred gammaray luminosity of the order of 1035erg/s, implications for the efficiency of converting available kinetic energy into non-thermal radiation associated with stellar winds in the Westerlund 2 cluster are discussed under consideration of either the presence or absence of wind clumping.},
  language  = {en}
}
@inproceedings{Kholtygin2007,
  author    = {Kholtygin, A. F.},
  title     = {Modelling the induced clumping stochastic line profile variability},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18180},
  year      = {2007},
  abstract  = {We model the line profile variability (lpv) in spectra of clumped stellar atmospheres using the Stochastic Clump Model (SCM) of the winds of early-type stars. In this model the formation of dense inhomogeneities (clumps) in the line driven winds is considered as being a stochastic process. It is supposed that the emission due to clumps mainly contributes to the intensities of emission lines in the stellar spectra. It is shown that in the framework of the SCM it is possible to reproduce both the mean line profiles and a common pattern of the lpv.},
  language  = {en}
}
@inproceedings{CheneMoffatCrowther2007,
  author    = {Chen{\´e}, A.-N. and Moffat, Anthony F. J. and Crowther, P. A.},
  title     = {Rapidly accelerating clumps in the winds of the very hot WNE Stars},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-18163},
  year      = {2007},
  abstract  = {We study the time variability of emission lines in three WNE stars : WR 2 (WN2), WR 3 (WN3ha) and WR152 (WN3). While WR 2 shows no variability above the noise level, the other stars do show variation, which are like other WR stars in WR 152 but very fast in WR 3. From these motions, we deduce a value of β ∼1 for WR 3 that is like that seen in O stars and β ∼2-3 for WR 152, that is intermediate between other WR stars and WR 3.},
  language  = {en}
}