A rotating, magnetic, radiation-driven wind model applied to Be stars

Details A rotating, magnetic, radiation-driven wind model applied to Be stars A rotating, magnetic, radiation-driven wind model applied to Be stars

Dec 1986

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1986apj...311..317p&link_type=abstract

Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 311, Dec. 1, 1986, p. 317-325.

Astronomy and Astrophysics

Astrophysics

82

B Stars, Magnetic Stars, Stellar Radiation, Stellar Rotation, Stellar Winds, Field Strength, O Stars, Radial Velocity, Stellar Mass Ejection, Terminal Velocity

Scientific paper

The rotating magnetic hot star wind model of Friend and MacGregor (1984) is extended to include the treatment of an O or Be star as a finite disk. In O stars, the mass-loss rates become nearly independent of the surface magnetic field strength. In Be stars, rapid rotation sharply increases the mass-loss rate and, for magnetic fields on the order of 50 G or less, decreases the terminal velocity. If the poles of a Be star are identified with low rotation rate models and the equator with high rotation rate models, then the rotating wind model predicts that the equator will have a slower and denser wind then the poles. This model is consistent with observations that the mass-loss rate along the equator is orders of magnitude larger than the rate near the poles. However, the velocity law on the equator still reaches the terminal velocity within a few stellar radii, in contradiction to the slowly expanding disk suggested by the empirical models of H-alpha emission and infrared excess.

Affiliated with

Also associated with

No associations

Rating

A rotating, magnetic, radiation-driven wind model applied to Be stars does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with A rotating, magnetic, radiation-driven wind model applied to Be stars, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and A rotating, magnetic, radiation-driven wind model applied to Be stars will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-1121383