The formation of outflowing disks around early-type stars by bi-stable radiation-driven winds

Details The formation of outflowing disks around early-type stars by bi-stable radiation-driven winds The formation of outflowing disks around early-type stars by bi-stable radiation-driven winds

Apr 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991a%26a...244l...5l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 244, no. 1, April 1991, p. L5-L8. University of Wisconsin-supported research.

Astronomy and Astrophysics

Astrophysics

123

Balmer Series, Early Stars, Emission Spectra, Stellar Winds, Supergiant Stars, Astronomical Models, Optical Thickness, Stellar Luminosity, Stellar Motions, Stellar Temperature

Scientific paper

A proposal is made to explain the existence of outflowing disks of rapidly rotating B-stars by means of the bistability mechanism of radiation driven winds. If the wind from a rotating B-star reaches an optical depth in the Lyman continuum at 912 A of tau(L) about 3 between the pole and the equator, the star will have a high velocity wind of high ionization in the polar regions and a low velocity wind of low ionization and high density near the equator. The strong dependence of tau(L) on stellar latitude makes the occurrence of such disks around rotating B-stars likely. The bistability mechanism can explain the major characteristics of the winds and disks of B(e)-supergiants and Be-stars and, in combination with some other mechanism, the variations of Be-stars into Be, B-shell and B-normal phases. It also explains why the outflowing disks occur mainly around early-B stars.

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