Viscous Transonic Outflow in Equatorial Discs of Be Stars

Details Viscous Transonic Outflow in Equatorial Discs of Be Stars Viscous Transonic Outflow in Equatorial Discs of Be Stars

Jan 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997cokon.100..407o&link_type=abstract

Communications of the Konkoly Observatory, No. 100 (Vol. XII, 2), p. 407-412 (1997)

Physics

Scientific paper

We discuss the characteristics of the outflow in discs of Be stars, based on the viscous decretion disc scenario. Solving the wind equation, we find that a transonic solution exists for any alpha. The sonic point is located at r > 100R for plausible values of parameters, where R is the stellar radius. The sonic radius is smaller for higher temperature and/or larger radiative force. We also find that the topology of the sonic point is nodal for alpha >~ 0.95, while it is saddle type for alpha <~ 0.9. In the subsonic region, the outflow velocity increases as r and the surface density decreases as r^-2. The angular velocity of the disc decreases as r^-1/2 in the inner subsonic region, while it decreases as r^-1 in the outer subsonic region.

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