X-ray Observations of Quiescent Recurrent Novae in CVs
Abstract
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.
- Publication:
-
XMM-Newton Proposal
- Pub Date:
- October 2009
- Bibcode:
- 2009xmm..prop..107M
- Keywords:
-
- White Dwarf Binaries;
- Neutron Star Binaries;
- Cataclysmic Variables;
- ULXs;
- Black Holes;
- V394 CrA;
- CI Aql