Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2010
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21530106w&link_type=abstract
American Astronomical Society, AAS Meeting #215, #301.06; Bulletin of the American Astronomical Society, Vol. 42, p.297
Astronomy and Astrophysics
Astronomy
Scientific paper
Negative superhumps in cataclysmic variable systems result when the accretion disk is tilted with respect to the orbital plane. The line of nodes of the tilted disk precesses slowly in the retrograde direction, resulting in a photometric signal with a period slightly less than the orbital period. Positive or common superhumps result when a disk is driven to oscillate near the 3:1 co-rotation resonance, yielding a period slightly in excess of the orbital period. We use the method of smoothed particle hydrodynamics to simulate a series of models of differing mass ratio and effective viscosity to determine the negative superhump period deficit ɛ- and positive superhump period excess ɛ+ as a function of system mass ratio q. We tabulate our results and present fits to both ɛ- and ɛ+ versus q, as well as compare the numerical results with those compiled from the literature of superhump observations. One surprising is that while we find negative superhumps most clearly in simulations with an accretion stream present, we also find evidence for negative superhumps in simulations in which we shut off the mass transfer stream completely, indicating that the origin of the photometric signal is more complicated than previously believed.
The lead author was on sabbatical from the Florida Institute of Technology (FIT) during the period of this work, and thanks Radboud University and The Netherlands Organisation for Scientific Research (NWO) for support through Visitor's Grant 040.11.046. This was supported in part by the National Science Foundation through grants AST-0205902 and AST-0552798.
Simpson James C.
Thomas David M.
Wood Matthew A.
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