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  • Clumping in stellar winds of hot stars is a possible consequence of radiative-acoustic instability appearing in solutions of radiative-hydrodynamical equations. However, clumping is usually included into stellar atmosphere modeling and radiative transfer calculations in a highly approximate way via a global free parameter called the clumping factor. Using different values of clumping factors, many researchers succeeded to fit the observed spectra better and to correct empirical mass-loss rates. This usually leads to a conclusion that the stellar wind is clumped. To understand how clumping may influence theoretical predictions of mass-loss rates, different clumping properties have to be taken into account. If clumping appears already below the critical point, the mass-loss rate is changed.
  • Clumping in stellar winds of hot stars is a possible consequence of radiative-acoustic instability appearing in solutions of radiative-hydrodynamical equations. However, clumping is usually included into stellar atmosphere modeling and radiative transfer calculations in a highly approximate way via a global free parameter called the clumping factor. Using different values of clumping factors, many researchers succeeded to fit the observed spectra better and to correct empirical mass-loss rates. This usually leads to a conclusion that the stellar wind is clumped. To understand how clumping may influence theoretical predictions of mass-loss rates, different clumping properties have to be taken into account. If clumping appears already below the critical point, the mass-loss rate is changed. (en)
Title
  • Validity of Clumping Approximations for Mass-Loss Rates Determination
  • Validity of Clumping Approximations for Mass-Loss Rates Determination (en)
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  • Validity of Clumping Approximations for Mass-Loss Rates Determination
  • Validity of Clumping Approximations for Mass-Loss Rates Determination (en)
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  • RIV/67985815:_____/12:00439737!RIV15-AV0-67985815
http://linked.open...avai/riv/aktivita
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  • I
http://linked.open...vai/riv/dodaniDat
http://linked.open...aciTvurceVysledku
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http://linked.open...iv/duvernostUdaju
http://linked.open...titaPredkladatele
http://linked.open...dnocenehoVysledku
  • 176910
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  • RIV/67985815:_____/12:00439737
http://linked.open...riv/jazykVysledku
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  • hot-star winds; driven stellar winds; bright ob-stars (en)
http://linked.open.../riv/klicoveSlovo
http://linked.open...ontrolniKodProRIV
  • [7B3459915B57]
http://linked.open...v/mistoKonaniAkce
  • Auberge Lac Taureau
http://linked.open...i/riv/mistoVydani
  • San Francisco
http://linked.open...i/riv/nazevZdroje
  • Four Decades of Research On Massive Stars
http://linked.open...in/vavai/riv/obor
http://linked.open...ichTvurcuVysledku
http://linked.open...cetTvurcuVysledku
http://linked.open...UplatneniVysledku
http://linked.open...iv/tvurceVysledku
  • Kubát, Jiří
  • Šurlan, Brankica
http://linked.open...vavai/riv/typAkce
http://linked.open...ain/vavai/riv/wos
  • 000316716000023
http://linked.open.../riv/zahajeniAkce
number of pages
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  • Astronomical Society of the Pacific
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  • 978-1-58381-812-1
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