| Issue |
A&A
Volume 570, October 2014
|
|
|---|---|---|
| Article Number | A4 | |
| Number of page(s) | 3 | |
| Section | Stellar structure and evolution | |
| DOI | https://doi.org/10.1051/0004-6361/201424357 | |
| Published online | 06 October 2014 | |
Research Note
The applicability of the wind compression model
Astronomical Institute, Slovak Academy of Sciences 059 60 Tatranská Lomnica Slovakia
e-mail:
zcarikova@ta3.sk
Received: 9 June 2014
Accepted: 22 August 2014
Compression of the stellar winds from rapidly rotating hot stars is described by the wind compression model. However, it was also shown that rapid rotation leads to rotational distortion of the stellar surface, resulting in the appearance of non-radial forces acting against the wind compression. In this note we justify the wind compression model for moderately rotating white dwarfs and slowly rotating giants. The former could be conducive to understanding density/ionization structure of the mass outflow from symbiotic stars and novae, while the latter can represent an effective mass-transfer mode in the wide interacting binaries.
Key words: stars: activity / stars: winds, outflows
© ESO, 2014
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