Physics
Scientific paper
Nov 1994
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994ap%26ss.221..443b&link_type=abstract
Astrophysics and Space Science (ISSN 0004-640X), vol. 221, no. 1-2, p. 443-453
Physics
2
Hot Stars, Stellar Mass, Stellar Models, Stellar Physics, Stellar Rotation, Stellar Winds, Accretion Disks, Flow Equations, H Alpha Line, Linear Polarization, Mass Distribution, Shock Waves, Stellar Evolution
Scientific paper
We discuss the structure of a radiatively-driven wind from a rapidly rotating hot star. When the rotation rate is large, there is a region at low latitudes near the stellar surface where the force of gravity is larger than the radiation pressure. Within this region, the streamlines 'fall' toward the equator, and if the rotation rate is large enough, the fluid collides with the flow from the opposite hemisphere of the star. The shock compression and subsequent cooling produces a dense equatorial disk. This wind-compressed disk forms only if the star is rotating fast enough. If theoretical calculations of the terminal speed are correct, then the behavior of the disk formation threshold as a function of spectral type potentially explains the frequency distribution of Be stars. The geometry of the wind-compressed disk agrees quite well with observations of Be stars; however, the disk density is a factor of 100 too small to explain the magnitude of the IR excess, optical polarization, and H-alpha emission, if current UV mass-loss rates are correct.
No associations
LandOfFree
Effects of rotation on hot star winds 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 Effects of rotation on hot star winds, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Effects of rotation on hot star winds will most certainly appreciate the feedback.
Profile ID: LFWR-SCP-O-1021765