Hydrodynamic calculations of accretion discs in close binaries. The superhump phenomenon

Details Hydrodynamic calculations of accretion discs in close binaries. The superhump phenomenon Hydrodynamic calculations of accretion discs in close binaries. The superhump phenomenon

Aug 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...288..807h&link_type=abstract

Astronomy and Astrophysics 288, 807-818 (1994)

Astronomy and Astrophysics

Astrophysics

27

Hydrodynamics, Instabilities, Accretion Discs, Cataclysmic Variables

Scientific paper

We have calculated the hydrodynamic evolution of an accretion disc in a close binary system with a low mass ratio in order to study the superhump phenomenon. We have tested the mode-coupling model of Lubow (1991a, 1991b) and find simular results if only the m=3 component of the tidal potential is used during the simulations. In case the full potential of the companion star is used, no eccentric prograde accretion disc evolves. The effective disc radii we infer from our simulations are approximately 70% of the Roche radius. These accretion discs are too small to become eccentric via the model of Lubow.

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