X-ray Observations of Quiescent Recurrent Novae in CVs

Details X-ray Observations of Quiescent Recurrent Novae in CVs X-ray Observations of Quiescent Recurrent Novae in CVs

Oct 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009xmm..prop..107m&link_type=abstract

XMM-Newton Proposal ID #06527602

Physics

White Dwarf Binaries, Neutron Star Binaries, Cataclysmic Variables, Ulxs, Black Holes, V394 Cra, Ci Aql

Scientific paper

For a binary to be a recurrent nova (RN), it must contain a massive white dwarf (WD) near the Chandrasekhar limit, making it a candidate progenitor of type Ia supernova. Although the WD masses and the accretion rates in RNe must all be similarly high, the X-ray properties of RNe with red-giant donar stars can be wildly different, ranging from hard and luminous (~1e34 ergs/s) to softer and significantly fainter (below 1e32 ergs/s). Such drastic differences may indicate that a third parameter, such as the spin period or the core temperature of the WD, may play an important role. Here we propose quiescent X-ray observations of 4 RNe in cataclysmicvariable (CV) systems to test if a third parameter indeed exists.

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