Mass transfer by tidally induced spiral shocks in an accretion disk

Details Mass transfer by tidally induced spiral shocks in an accretion disk Mass transfer by tidally induced spiral shocks in an accretion disk

Aug 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990a%26a...235..211m&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 235, no. 1-2, Aug. 1990, p. 211-218. Research supported by the Institute of Sp

Statistics

Computation

33

Accretion Disks, Binary Stars, Shock Waves, Stellar Mass Accretion, Computational Astrophysics, Radiative Transfer, Tides

Scientific paper

Numerical simulations are presented of the evolution of disks in binary systems under the influence of accretion through spiral shock waves. The calculations are followed for at least one radial drift time scale, thereby improving upon previous results. The accretion time scale (radial drift time from the outer edge of the disk) decreases from about 1000 orbital periods at a mass ratio of 1000 to about 15 orbits at q = 0.1. Due to the neglect of radiative losses the disks studied are still significantly hotter than realistic disks, however.

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