Optically thick radial accretion onto main sequence stars and degenerate dwarfs

Details Optically thick radial accretion onto main sequence stars and degenerate dwarfs Optically thick radial accretion onto main sequence stars and degenerate dwarfs

Jun 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...147..197t&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 147, no. 2, June 1985, p. 197-201.

Astronomy and Astrophysics

Astrophysics

6

Dwarf Stars, Main Sequence Stars, Stellar Mass Accretion, Symbiotic Stars, T Tauri Stars, Optical Thickness, Stellar Magnitude, Stellar Mass, Stellar Temperature

Scientific paper

At a sufficiently large rate, radial accretion flow becomes so opaque that a sort of effective photosphere is formed in the free-falling matter above the hydrostatic stellar surface. A simple method which makes it possible to determine the radius and temperature of the effective photosphere for an optically thick flow is presented. If M(T) is defined as the accretion rate at which the transition between the optically thin and optically thick regimes occurs, then for main-sequence stars M(T) = 0.001 M(Edd). In the case of degenerate dwarfs, M(T) is a function of the dwarf mass and varies from 0.005 M(Edd) for 0.15 solar mass to 0.5 M(Edd) for 1.35 solar mass. It is suggested that YY Orionis stars accrete at a rate close to M(T). In binary systems radial accretion onto a main-sequence star or a degenerate dwarf from the strong variable anisotropic wind of an M giant companion may lead to phenomena similar to those observed in symbiotic stars.

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