Hydrodynamic simulations of accretion disks in cataclysmic variables - Superhump phenomenon in SU UMa stars

Details Hydrodynamic simulations of accretion disks in cataclysmic variables - Superhump phenomenon in SU UMa stars Hydrodynamic simulations of accretion disks in cataclysmic variables - Superhump phenomenon in SU UMa stars

Feb 1990

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1990pasj...42..135h&link_type=abstract

Astronomical Society of Japan, Publications (ISSN 0004-6264), vol. 42, no. 1, 1990, p. 135-163.

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180

Accretion Disks, Cataclysmic Variables, Dwarf Novae, Hydrodynamics, Stellar Mass Accretion, Computational Astrophysics, Gravitational Fields, Red Dwarf Stars, Stellar Orbits, Stellar Rotation, White Dwarf Stars

Scientific paper

The tidal effects of secondary stars on accretion disks in cataclysmic variables are studied by two-dimensional hydrodynamical simulations. The time evolution of an accretion disk under a constant mass supply rate from the secondary is followed until it reaches a quasi-steady state. It is found that the accretion disk settles into a steady state of an elongated disk fixed in the rotating frame of the binary in a binary system with comparable masses of component stars. On the other hand, in the case of a low-mass secondary, the accretion disk develops a non-axisymmetric (eccentric) structure and finally settles into a periodically oscillating state in which a non-axisymmetric eccentric disk rotates in the opposite direction to the orbital motion of the binary in the rotating frame of the binary. The period of oscillation is a few percent longer than the orbital period of the binary, and it offers a natural explanation for the superhump periodicity of SU UMa stars.

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