@misc{KubatovaKubatHamannetal.2017,
  author    = {Kubatova, B. and Kub{\´a}t, Jiř{\´i} and Hamann, Wolf-Rainer and Oskinova, Lida},
  title     = {Clumping in Massive Star Winds and its Possible Connection to the B[e] Phenomenon},
  series = {The B(e) Phenomenon: Forty Years of Studies : proceedings of a conference held at Charles University, Prague, Czech Republic, 27 June-1 July 2016},
  volume    = {508},
  journal   = {The B(e) Phenomenon: Forty Years of Studies : proceedings of a conference held at Charles University, Prague, Czech Republic, 27 June-1 July 2016},
  publisher = {Astronomical Soceity of the Pacific},
  address   = {San Fransisco},
  isbn      = {978-1-58381-900-5},
  pages     = {45 -- 50},
  year      = {2017},
  abstract  = {It has been observationally established that winds of hot massive stars have highly variable characteristics. The variability evident in the winds is believed to be caused by structures on a broad range of spatial scales. Small-scale structures (clumping) in stellar winds of hot stars are possible consequence of an instability appearing in their radiation hydrodynamics. To understand how clumping may influence calculation of theoretical spectra, different clumping properties and their 3D nature have to be taken into account. Properties of clumping have been examined using our 3D radiative transfer calculations. Effects of clumping for the case of the B[e] phenomenon are discussed.},
  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}
}
@article{VotrubaFeldmeierKrtickaetal.2010,
  author    = {Votruba, Viktor and Feldmeier, Achim and Krticka, Jiri and Kub{\´a}t, Jiř{\´i}},
  title     = {Multicomponent stellar wind from hot subdwarfs stars},
  issn      = {0004-640X},
  doi       = {10.1007/s10509-010-0402-2},
  year      = {2010},
  abstract  = {Stellar wind from hot subdwarf stars is mainly accelerated by the interaction of ultraviolet photospheric radiation with metals, mainly oxygen. Absorbing ions share momentum through Coulombic collisions with the remaining passive part of the plasma (namely protons). We found that in the case of the winds from hot subdwarfs, interactions could be so small that they stop the momentum transfer between the passive bulk of plasma and absorbing ions. As a result wind decouples at a certain point.},
  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{KrtičkaPulsKubat2007,
  author    = {Krtička, Jiri and Puls, Joachim and Kub{\´a}t, Jiř{\´i}},
  title     = {The influence of clumping on predicted O star wind parameters},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17969},
  year      = {2007},
  abstract  = {We study the influence of clumping on the predicted wind structure of O-type stars. For this purpose we artificially include clumping into our stationary wind models. When the clumps are assumed to be optically thin, the radiative line force increases compared to corresponding unclumped models, with a similar effect on either the mass-loss rate or the terminal velocity (depending on the onset of clumping). Optically thick clumps, alternatively, might be able to decrease the radiative force.},
  language  = {en}
}
@inproceedings{KrausKubatKrtička2007,
  author    = {Kraus, M. and Kub{\´a}t, Jiř{\´i} and Krtička, Jiri},
  title     = {Wind emission of OB supergiants and the influence of clumping},
  url       = {http://nbn-resolving.de/urn:nbn:de:kobv:517-opus-17757},
  year      = {2007},
  abstract  = {The influence of the wind to the total continuum of OB supergiants is discussed. For wind velocity distributions with β > 1.0, the wind can have strong influence to the total continuum emission, even at optical wavelengths. Comparing the continuum emission of clumped and unclumped winds, especially for stars with high β values, delivers flux differences of up to 30\% with maximum in the near-IR. Continuum observations at these wavelengths are therefore an ideal tool to discriminate between clumped and unclumped winds of OB supergiants.},
  language  = {en}
}