Astronomy and Astrophysics – Astronomy
Scientific paper
Oct 2007
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007arep...51..847t&link_type=abstract
Astronomy Reports, Volume 51, Issue 10, pp.847-862
Astronomy and Astrophysics
Astronomy
3
97.30.Eh, 97.10.Cv, 97.10.Bt, 97.10.Gz, 97.10.Me, Emission-Line Stars, Stellar Structure, Interiors, Evolution, Nucleosynthesis, Ages, Star Formation, Accretion And Accretion Disks, Mass Loss And Stellar Winds
Scientific paper
Several scenarios for the formation of accretion and decretion disks in single and binary Ae and Be stars are proposed. It is shown that, in order for a rapidly rotating main-sequence Be star to lose mass via a disk, the star’s rotation must be quasi-rigid-body. Estimates show that such rotation can be maintained by the star’s magnetic field, which is probably a relict field. The evolution of single Be main-sequence stars is numerically simulated allowing for mass loss via the stellar wind and rotational mass loss assuming rigid-body rotation. The stellar wind is the factor that determines the maximum mass of Be stars, which is close to 30 M &sun;. The evolution of Be stars in close binaries is analyzed in the approximation adopted in our scenario. Long gamma-ray bursts can be obtained as a result of the collapse of rapidly rotating oxygen—neon degenerate dwarfs—the accreting companions of Be stars—into neutron stars.
Fedorova Alexandra V.
Tutukov Aleksandr V.
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