A Parametric Study of Cataclysmic Variable Superhump Oscillations

Details A Parametric Study of Cataclysmic Variable Superhump Oscillations A Parametric Study of Cataclysmic Variable Superhump Oscillations

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...195.4002b&link_type=abstract

American Astronomical Society, 195th AAS Meeting, #40.02; Bulletin of the American Astronomical Society, Vol. 31, p.1428

Astronomy and Astrophysics

Astronomy

Scientific paper

We simulate cataclysmic variable disk superhump oscillations for systems with mass ratios q=M2/M_1 in the range 0.03 < q < 0.30 using a three-dimensional smoothed particle hydrodynamics (SPH) code. We report the preliminary results from this parametric study in which over 4000 system orbits were calculated. In each run we start with an empty disk, build it rapidly to N=25,000 particles in 12.5 orbits, and then hold N at this value by replacing accreted particles at the L1 point. Thus, our models most closely resemble the permanent superhumping systems. Our resulting superhump period-excess versus orbital period relation agrees well with the observations, as do the mean pulse profiles. The superhump oscillation periods do not appear to be a strong function of viscosity, although the oscillations take fewer orbits to devlop in the high viscosity disks. We find superhumps develop most rapidly in systems with q=0.075, and progressively later as the mass ratio approaches the extremes of q=0.03 and 0.30. This work was funded by the NSF through the SARA Research Experiences for Undergraduates Summer Internship Program (NSF AST--9619939).

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