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 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007xmm..prop..183s&link_type=abstract

XMM-Newton Proposal ID #05560402

Computer Science

White Dwarf Binaries, Neutron Star Binaries, Cataclysmic Variables, Ulxs, Black Holes, V3890 Sgr, V745 Sco, Xmm-Newton Proposal Id #05560402

Scientific paper

Recurrent nova (RN) contain white dwarfs whose masses are close to the Chandrasekhar limit. Some RN may thus be progenitors of type Ia supernovae (SNIa). In fact, recent observations by Patat et al. of circumstellar material in a normal SNIa suggest that massive WDs accreting from a red-giant companion can give rise to SNIa. To test the idea that hard X-ray emission, which is seen from several high-mass WDs accreting from red-giant companions, is a marker for SNIa progenitors, and to probe the nature of accretion in the last stages before SNIa explosion, we propose to observe two of the four RN with giant companions -- V3890 Sgr and V745 Sco -- both of which we consider to be good SNIa progenitor candidates.

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