Rapid mass accretion on a fully convective star

Details Rapid mass accretion on a fully convective star Rapid mass accretion on a fully convective star

Mar 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987ap%26ss.131..671s&link_type=abstract

(IAU, Colloquium on Cataclysmic Variables. Recent Multi-Frequency Observations and Theoretical Developments, 93rd, Bamberg, West

Astronomy and Astrophysics

Astrophysics

1

Convective Heat Transfer, Main Sequence Stars, Stellar Magnitude, Stellar Mass Accretion, Stellar Structure, Stellar Cores, Stellar Envelopes, Temperature Inversions

Scientific paper

The effects of rapid mass accretion on a fully convective main sequence star of 0.3 solar masses are investigated, taking into account the heating of its photosphere by the kinetic energy of the infalling matter. It is found that the star develops a highly inhomogeneous structure consisting of an almost unperturbed initial convective core and a radiative envelope composed of the accreted matter. Both regions are separated by a very stable temperature inversion layer. Due to such a structure, an accreting convective star may significantly increase its radius (contrary to earlier suggestions).

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