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The Possibility of a Disk Formation around Late B Stars

Published online by Cambridge University Press:  26 May 2016

Jiří Kubát ,
Jiří Krtička ,
Izold B. Pustylnik  and
Viktor Votruba
Jiří Kubát
Affiliation:
Astronomický ústav AV ČR, CZ-251 65 Ondřejov, Czech Republic
Jiří Krtička
Affiliation:
Astronomický ústav AV ČR, CZ-251 65 Ondřejov, Czech Republic Department of Physics and Astronomy, University of Glasgow, Glasgow G12 8QQ, UK Ústav teoretické fyziky a astrofyziky Přf MU, Kotlářská 2, CZ-611 37 Brno, Czech Republic
Izold B. Pustylnik
Affiliation:
Tartu Observatory, 61602 Tõravere, Estonia
Viktor Votruba
Affiliation:
Astronomický ústav AV ČR, CZ-251 65 Ondřejov, Czech Republic Ústav teoretické fyziky a astrofyziky Přf MU, Kotlářská 2, CZ-611 37 Brno, Czech Republic

Abstract

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Line driven wind in late B stars causes significant heating of layers just above the photosphere. This large heating is a source of a thermal wind, which together with fast rotation opens the possibility of a formation of a disk. We refer to such disk as to a radiation induced disk. Disk inhibition by nonradial line force has only little effect in this case, since absorption in spectral lines is not the main wind driving mechanism.

Type
Session 1 Observations of Rotating Stars
Information
Symposium - International Astronomical Union , Volume 215: Stellar Rotation , 2004 , pp. 49 - 50
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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