Hydrodynamic simulations of cataclysmic variable accretion discs in outburst

Details Hydrodynamic simulations of cataclysmic variable accretion discs in outburst Hydrodynamic simulations of cataclysmic variable accretion discs in outburst

Apr 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999mnras.304..687s&link_type=abstract

Monthly Notices of the Royal Astronomical Society, Volume 304, Issue 3, pp. 687-697.

Astronomy and Astrophysics

Astronomy

17

Accretion, Accretion Discs, Shock Waves, Binaries: Close, Novae, Cataclysmic Variables

Scientific paper

We study the outburst phase of cataclysmic variable (CV) accretion discs in the (r, pi) plane with full hydrodynamics. Vertically the disc is treated using the one-zone model of Stehle & Spruit, which allows us to follow the fundamental mode of vertical disc oscillations correctly. alpha-type shear viscosity (Shakura & Sunyaev) and energy loss at the surface of the accretion disc by radiation are included. We run accretion disc models with different masses M_1 and M_2 for the primary and the secondary stars and different values of alpha. In all calculations we observe strong spiral shock arms, which dominate the disc evolution on a hydrodynamical time-scale. In cases where the surface mass density Sigma (r) decreases with radius r the disc pattern is stable. In cases where Sigma (r) increases with r we observe a quasi-periodic cycle of disc size. During the phase where the disc is large, the spiral arm close to the L_1 point connects to the secondary, and about 1 per cent of the total disc mass is lost to the secondary per cycle. However, in none of our calculations are we able to find an eccentric and precessing accretion disc, even though the disc edge is outside the 3:1 tidal resonance radius R_31. Our calculations therefore cannot confirm the tidal instability model, presently the only model for superhumps in SU UMa CVs during superoutbursts.

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