@inproceedings{Kholtygin2007,
  author    = {Kholtygin, A. F.},
  title     = {Wavelets for looking for clumping in the wind of OB stars},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17796},
  year      = {2007},
  abstract  = {Clumping in hot-star winds : proceedings of an international workshop held in Potsdam, Germany, 18. - 22. June 2007},
  language  = {en}
}
@inproceedings{ReyesIturbideVelazquezRosado2007,
  author    = {Reyes-Iturbide, J. and Vel{\´a}zquez, P. and Rosado, M.},
  title     = {3D numerical model for an asymmetrical superbubble},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17724},
  year      = {2007},
  abstract  = {Massive stars usually form groups such as OB associations. Their fast stellar winds sweep up collectively the surrounding insterstellar medium (ISM) to generate superbubbles. Observations suggest that superbubble evolution on the surrounding ISM can be very irregular. Numerical simulations considering these conditions could help to understand the evolution of these superbubbles and to clarify the dynamics of these objects as well as the difference between observed X-ray luminosities and the predicted ones by the standard model (Weaver et al. 1977).},
  language  = {en}
}
@inproceedings{VotrubaFeldmeierKubatetal.2007,
  author    = {Votruba, V. and Feldmeier, Achim and Kub{\´a}t, Jiř{\´i} and R{\"a}tzel, D.},
  title     = {Multicomponent stellar wind of hot stars},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17677},
  year      = {2007},
  abstract  = {We developed a time-dependent multicomponent hydrodynamical code for simulation of the stellar wind from hot stars and applied it to stars with high and low density winds.},
  language  = {en}
}
@inproceedings{LiermannHamann2007,
  author    = {Liermann, A. and Hamann, Wolf-Rainer},
  title     = {Clumping in Galactic WN stars : a comparison of mass loss rates from UV/optical \& radio diagnostics},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17816},
  year      = {2007},
  abstract  = {The mass loss rates and other parameters for a large sample of Galactic WN stars have been revised by Hamann et al. (2006), using the most up-to date Potsdam Wolf-Rayet (PoWR) model atmospheres. For a sub-sample of these stars exist measurements of their radio free-free emission. After harmonizing the adopted distance and terminal wind velocities, we compare the mass loss rates obtained from the two diagnostics. The differences are discussed as a possible consequence of different clumping contrast in the line-forming and radio-emitting regions.},
  language  = {en}
}
@inproceedings{RaassenHuchtMilleretal.2007,
  author    = {Raassen, A. J. J. and Hucht, K. A. van der and Miller, N. A. and Cassinelli, Joseph P.},
  title     = {XMM-Newton observations of zeta Orionis (O9.7 Ib) : a collisional ionization equilibrium model},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17747},
  year      = {2007},
  abstract  = {We present the analysis of XMM-Newton observations of ζ Orionis. The analysis is based on fitting to the total spectrum as well as diagnostics of individual line.},
  language  = {en}
}
@inproceedings{IpingSonnebornMassaetal.2007,
  author    = {Iping, R.C. and Sonneborn, G. and Massa, D.L. and Gies, D. and Williams, Simon E.},
  title     = {Far-ultraviolet spectroscopy of O+O binaries in the Magellanic Clouds},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17896},
  year      = {2007},
  abstract  = {We report FUSE observations in 2005-2006 of three O-type, double-lined spectroscopic binaries in the Magellanic Clouds. The systems have very short periods (1.4-2.25 d), represent rare, young evolutionary stages of massive stars and binaries, and provide a unique glimpse at some of the most massive systems that form in dense clusters of massive stars. Improved orbit parameters, including revised masses, for LH54-425 are derived from new ctio spectroscopy. The systems are: LH54-425 in the LMC (O3V + O5V, P=2.25d, 62+37M⊙), J053441-693139 in the LMC (O2-3If+O6V, P=1.4 d, 41+27M⊙), and Hodge 53-47 in the SMC (O6V + O4-5IIIf, P=2.2 d, 24+14M⊙, where the O4 star appears to be less massive than the O6 star). Their short periods indicates that wind interaction and mass transfer are likely important factors in their evolution. The spectra provide quantitative and systematic studies of phase-dependent stellar wind properties, wind collision effects in O+O binaries at lower metallicities, improved radial velocity curves, and FUV spectro-photometric changes as a function of orbital phase.},
  language  = {en}
}
@inproceedings{KustererNagelWerneretal.2007,
  author    = {Kusterer, D.-J. and Nagel, T. and Werner, K. and Feldmeier, Achim},
  title     = {Radiative transfer in CV disk winds},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17847},
  year      = {2007},
  abstract  = {Mass accretion onto compact objects through accretion disks is a common phenomenon in the universe. It is seen in all energy domains from active galactic nuclei through cataclysmic variables (CVs) to young stellar objects. Because CVs are fairly easy to observe, they provide an ideal opportunity to study accretion disks in great detail and thus help us to understand accretion also in other energy ranges. Mass accretion in these objects is often accompanied by mass outflow from the disks. This accretion disk wind, at least in CVs, is thought to be radiatively driven, similar to O star winds. WOMPAT, a 3-D Monte Carlo radiative transfer code for accretion disk winds of CVs is presented.},
  language  = {en}
}
@inproceedings{DaviesVinkOudmaijer2007,
  author    = {Davies, B. and Vink, J. S. and Oudmaijer, R. D.},
  title     = {Modelling the polarimetric variability of hot stars},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17939},
  year      = {2007},
  abstract  = {Many hot stars exhibit stochastic polarimetric variability, thought to arise from clumping low in the wind. Here we investigate the wind properties required to reproduce this variability using analytic models, with particular emphasis on Luminous Blue Variables. We find that the winds must be highly structured, consisting of a large number of optically-thin clumps; while we find that the overall level of polarization should scale with mass-loss rate - consistent with observations of LBVs. The models also predict variability on very short timescales, which is supported by the results of a recent polarimetric monitoring campaign.},
  language  = {en}
}
@inproceedings{KubatSaad2007,
  author    = {Kub{\´a}t, Jiř{\´i} and Saad, S. M.},
  title     = {Moving absorption bumps in the spectra of Be stars},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17879},
  year      = {2007},
  abstract  = {Several Be binaries exhibit an absorption bump moving across the blue wing of hydrogen emission lines towards the line center. This bump is demonstrated for the case of two bright Be stars, κ Dra and 4 Her. It is not clear what is the reason for this travelling bump.},
  language  = {en}
}
@inproceedings{TodtHamannGraefener2007,
  author    = {Todt, Helge Tobias and Hamann, Wolf-Rainer and Gr{\"a}fener, G.},
  title     = {Clumping in [WC]-type Central Stars from electron-scattering line wings},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17711},
  year      = {2007},
  abstract  = {While there is strong evidence for clumping in the winds of massive hot stars, very little is known about clumping in the winds from Central Stars. We have checked [WC]-type CSPN winds for clumping by inspecting the electron-scattering line wings. At least for three stars we found indications for wind inhomogeneities.},
  language  = {en}
}