Viscous excretion discs around Be stars

Details Viscous excretion discs around Be stars Viscous excretion discs around Be stars

May 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991mnras.250..432l&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 250, May 15, 1991, p. 432-437.

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108

Angular Momentum, B Stars, Mass Flow, Stellar Mass Ejection, Viscosity, Computational Astrophysics, Stellar Models, Thermal Stability

Scientific paper

The present consideration of the characteristics of viscous, geometrically thin Keplerian excretion disks around Be stars, it is assumed that angular momentum is transferred by some mechanism from the interior to the equatorial surface of the central star; matter is therefore supplied at the inner boundary of the disk at a certain rate. In the case of mass excretion rates similar to the mass-loss rate estimated for Be stars, the irradiative heating by the central star is as essential for the disk structure as the viscous heating in the disk. It is demonstrated that the irradiated excretion disks around Be stars have a thermally unstable region, when the mass excretion rate is of the order of 10 to the -7th solar masses/yr.

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