Hard X-Ray Emission from Progenitors of Type Ia Supernovae
Abstract
Recurrent nova (RN) contain white dwarfs (WDs) whose masses are close to the Chandrasekhar limit. Some RN may thus be progenitors of type Ia supernovae (SNIa). But how do the WDs in these binaries accrete enough material to approach the Chandrasekhar limit? To address this question, and to develop a tool for finding SNIa progenitor candidates at an earlier stage along the path to the Chandrasekhar limit, we propose to test the degree to which hard X-ray emission is a marker for high WD mass. We thus propose to observe two RN that have no previous pointed X-ray observations in quiescence. Our targets both have red-giant mass donor stars, which makes them similar to the one RN known to produce strong, hard X-ray emission. This work is motivated in part by the advent of new hard X-ray surveys.
- Publication:
-
XMM-Newton Proposal
- Pub Date:
- October 2008
- Bibcode:
- 2008xmm..prop..139S
- Keywords:
-
- White Dwarf Binaries;
- Neutron Star Binaries;
- Cataclysmic Variables;
- ULXs;
- Black Holes;
- V3890 Sgr;
- V745 Sco