Hard X-Ray Emission from Progenitors of Type Ia Supernovae

Details Hard X-Ray Emission from Progenitors of Type Ia Supernovae Hard X-Ray Emission from Progenitors of Type Ia Supernovae

Oct 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009xmm..prop..122s&link_type=abstract

XMM-Newton Proposal ID #06534302

Physics

White Dwarf Binaries, Neutron Star Binaries, Cataclysmic Variables, Ulxs, Black Holes, V3890 Sgr, V745 Sco

Scientific paper

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). To develop a tool for finding SNIa progenitor candidates at an earlier stage along the path to the Chandrasekhar limit, and to constrain the properties of known candidate SNIa progenitors, we propose to test the degree to which hard X-ray emission is a marker for high WD mass. We will observe two RN that have no previous pointed X-ray observations in quiescence. We selected our targets because they have red-giant mass donor stars, which makes them similar to the one RN already known to produce strong, hard X-ray emission. This work is motivated in part by the advent of new hard X-ray surveys.

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