SPH simulations of late superhumps

Details SPH simulations of late superhumps SPH simulations of late superhumps

Jan 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002aspc..261..497k&link_type=abstract

The Physics of Cataclysmic Variables and Related Objects, ASP Conference Proceedings, Vol. 261. Edited by B. T. Gänsicke, K. Beu

Physics

1

Scientific paper

I present results of 3D SPH simulations of the accretion disk in the SU UMa system OY Car. During superoutburst, superhumps arise due to the precession of the eccentric disk. The return to quiescence is modelled by a decrease of the viscosity and the mass transfer rate. It turns out that the eccentricity of the disk vanishes only slowly, a modulation of the brightness with the superhump period is still present. These late superhumps are phase-shifted about 180deg. The source of the late superhump light is a modulation of the bright spot brightness, as more energy is released in this region when it is closer to the white dwarf.

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