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Synthetic spectra of A supergiants

Published online by Cambridge University Press:  02 March 2005

D. Korčáková ,
J. Kubát ,
J. Krtička  and
M. šlechta
D. Korčáková
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic, Fričova 298, CZ-251 65 Ondřejov, Czech Republic email: kor@sunstel.asu.cas.cz, kubat@sunstel.asu.cas.cz, slechta@sunstel.asu.cas.cz
J. Kubát
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic, Fričova 298, CZ-251 65 Ondřejov, Czech Republic email: kor@sunstel.asu.cas.cz, kubat@sunstel.asu.cas.cz, slechta@sunstel.asu.cas.cz
J. Krtička
Affiliation:
Institute of Theoretical Physics and Astrophysics, Masaryk University, Kotrlářská 2, CZ-611 37 Brno, Czech Republic email: krticka@physics.muni.cz
M. šlechta
Affiliation:
Astronomical Institute, Academy of Sciences of the Czech Republic, Fričova 298, CZ-251 65 Ondřejov, Czech Republic email: kor@sunstel.asu.cas.cz, kubat@sunstel.asu.cas.cz, slechta@sunstel.asu.cas.cz
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Abstract

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The stellar winds of A supergiants can have a significant influence on their emergent spectra. Here we present the hydrogen line profiles of a model based on the stellar parameters of HD 12953. The radiative transfer equation is solved in two dimensions in axial symmetry. We do not include the velocity field by the Sobolev approximation, but in detail using the Lorentz transformation. This allows us to correctly include the stellar wind, since the velocity gradients in A supergiants are too small for the Sobolev approximation to be valid.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Keywords

Hydrodynamicsline: profilesradiative transfer(stars:) supergiantsstars: individual (HD 12953)
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2004 , Issue IAUS224 , July 2004 , pp. 533 - 538
Copyright
© 2004 International Astronomical Union