KRTIČKA, Jiří and Jiří KUBÁT. Multicomponent radiatively driven stellar winds I.Nonisothermal three-component wind of hot B stars. Astronomy and Astrophysics. Les Ulis Cedex, France: EDP Sciences, vol. 35, No 369, p. 222-238. ISSN 0004-6361. 2001.
Other formats:   BibTeX LaTeX RIS
Basic information
Original name Multicomponent radiatively driven stellar winds I.Nonisothermal three-component wind of hot B stars
Authors KRTIČKA, Jiří (203 Czech Republic, guarantor) and Jiří KUBÁT.
Edition Astronomy and Astrophysics, Les Ulis Cedex, France, EDP Sciences, 2001, 0004-6361.
Other information
Original language English
Type of outcome Article in a journal
Field of Study 10308 Astronomy
Country of publisher France
Confidentiality degree is not subject to a state or trade secret
WWW URL
Impact factor Impact factor: 2.790 in 2000
RIV identification code RIV/00216224:14310/01:00004112
Organization unit Faculty of Science
Keywords in English hydrodynamics -- stars: mass-loss -- stars: early-type -- stars: winds -- stars: individual: tau Sco
Tags International impact, Reviewed
Changed by Changed by: prof. Mgr. Jiří Krtička, Ph.D., učo 8714. Changed: 5/3/2007 17:57.
Abstract
We computed models of a three-component nonisothermal radiatively driven stellar wind for different spectral types of hot B stars. We showed that friction heats mainly the outer parts of the wind and the modified temperature stratification leads to a decrease of the outflow velocity. Contrary to the isothermal case, even the possibility of decoupling of radiatively absorbing ions and (major) nonabsorbing component is excluded for a realistic form of the driving force. Regardless of the actual form of the driving force, we derived general conditions under which decoupling of a stellar wind may occur. We demonstrated that the possibility of decoupling is closely related to the functional dependence of the driving force and to the ratio of the densities of individual components. We discuss several consequences of a multifluid phenomenon in hot star winds, particularly metallicity effects and the implications of possible helium decoupling on chemically peculiar stars. We propose an explanation of the low terminal velocity of tau Sco based on frictional heating.
Links
GA205/01/0656, research and development projectName: Modelování rozsáhlých obálek horkých hvězd
PrintDisplayed: 28/3/2024 19:07