Implications of a Disk Instability in RS Ophiuchi

Details Implications of a Disk Instability in RS Ophiuchi Implications of a Disk Instability in RS Ophiuchi

Jan 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010aas...21541626c&link_type=abstract

American Astronomical Society, AAS Meeting #215, #416.26; Bulletin of the American Astronomical Society, Vol. 42, p.270

Astronomy and Astrophysics

Astronomy

Scientific paper

Recently King & Pringle have proposed that the 2006 outburst of the recurrent nova RS Oph is better explained in terms of a dwarf nova-type accretion disk instability rather than as a thermonuclear explosion on the surface of the WD primary. Using a numerical time dependent accretion disk model, we examine in detail the predictions and ramifications of the disk instability model for RS Oph, given its orbital period and putative mass transfer rate. Our findings are that an outburst due to an accretion disk instability would be fainter, longer, and vary more slowly than the observed outburst. However, in our most optimized model, the amount of mass accreted onto the WD is in line with that required in the thermonuclear runaway model, assuming a 1.4 Msol WD, therefore it may be that the disk instability is the trigger for a thermonuclear runaway.

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