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 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008xmm..prop..139s&link_type=abstract

XMM-Newton Proposal ID #06049802

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). 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.

Affiliated with

Also associated with

No associations

Rating

Hard X-Ray Emission from Progenitors of Type Ia Supernovae does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Hard X-Ray Emission from Progenitors of Type Ia Supernovae, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Hard X-Ray Emission from Progenitors of Type Ia Supernovae will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-866268