@misc{DolezalovaKubatovaKubatetal.2019,
  author    = {Dolezalova, Barbora and Kubatova, Brankica and Kubat, Jiri and Hamann, Wolf-Rainer},
  title     = {The Quasi-WR Star HD 45166 Revisited},
  series = {Radiative signatures from the cosmos},
  volume    = {519},
  journal   = {Radiative signatures from the cosmos},
  publisher = {Astronomical soc pacific},
  address   = {San Fransisco},
  isbn      = {978-1-58381-925-8},
  issn      = {1050-3390},
  pages     = {197 -- 200},
  year      = {2019},
  abstract  = {We studied the wind of the quasi Wolf-Rayet (qWR) star HD 45166. As a first step we modeled the observed UV spectra of this star by means of the state-of-the-art Potsdam Wolf-Rayet (PoWR) atmosphere code. We inferred the wind parameters and compared them with previous findings.},
  language  = {en}
}
@misc{KubatovaHamannKubatetal.2019,
  author    = {Kubatova, Brankica and Hamann, Wolf-Rainer and Kubat, Jiri and Oskinova, Lida},
  title     = {3D Monte Carlo Radiative Transfer in Inhomogeneous Massive Star Winds},
  series = {Radiative signatures from the cosmos},
  volume    = {519},
  journal   = {Radiative signatures from the cosmos},
  publisher = {Astronomical soc pacific},
  address   = {San Fransisco},
  isbn      = {978-1-58381-925-8},
  issn      = {1050-3390},
  pages     = {209 -- 212},
  year      = {2019},
  abstract  = {Already for decades it has been known that the winds of massive stars are inhomogeneous (i.e. clumped). To properly model observed spectra of massive star winds it is necessary to incorporate the 3-D nature of clumping into radiative transfer calculations. In this paper we present our full 3-D Monte Carlo radiative transfer code for inhomogeneous expanding stellar winds. We use a set of parameters to describe dense as well as the rarefied wind components. At the same time, we account for non-monotonic velocity fields. We show how the 3-D density and velocity wind inhomogeneities strongly affect the resonance line formation. We also show how wind clumping can solve the discrepancy between P v and H alpha mass-loss rate diagnostics.},
  language  = {en}
}