Rotating and selfgravitating winds.
Abstract
The paper considers a rotating star with an isothermal and stationary expanding corona whose gravitational potential cannot be neglected. As in ordinary wind theories, there exists a critical sonic point. The position of this critical point, the initial velocity of the gas, and the mass loss of the critical solution are calculated. These quantities depend on the gravitational binding and density of the corona as well as the rotation of the star (being represented by three dimensionless parameters). As long as the density of the corona is 'small', the mass loss is found to increase with increasing values of two of the rotation parameters; for 'high' density, a decrease occurs.
- Publication:
-
Astronomy and Astrophysics
- Pub Date:
- January 1976
- Bibcode:
- 1976A&A....46..213W
- Keywords:
-
- Stellar Gravitation;
- Stellar Mass Ejection;
- Stellar Rotation;
- Stellar Winds;
- Astronomical Models;
- Atmospheric Density;
- Numerical Integration;
- Solar Wind;
- Stellar Envelopes;
- Stellar Evolution;
- Subsonic Flow;
- Supersonic Flow;
- Astrophysics