Characterization and Evolution of the Supersoft X-ray Phase of Classical Novae

Details Characterization and Evolution of the Supersoft X-ray Phase of Classical Novae Characterization and Evolution of the Supersoft X-ray Phase of Classical Novae

Oct 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007xmm..prop..171s&link_type=abstract

XMM-Newton Proposal ID #05556913

Computer Science

White Dwarf Binaries, Neutron Star Binaries, Cataclysmic Variables, Ulxs, Black Holes, V390 Nor, V5558 Sgr, V1065 Cen, V2615 Oph, V2467 Cyg, V1280 Sco, V1281 Sco, Yy Dor, De Cir, V1187 Sco, V475 Sct, V5117 Sgr, V458 Vul, Xmm-Newton Proposal Id #05556913

Scientific paper

Outbursts of novae are driven by a thermonuclear runaway at the base of an accreted shell. Soft X-ray emission resulting from high surface temperatures on the WD after outburst are expected, but seldom observed (SSS phase). Some novae enter the SSS phase within a year after outburst, and quickly turn off thereafter (very fast ONeMg novae). Slow novae are delayed years after outburst before entering the SSS stage, which then last many years. ROSAT detected only 3 novae in their SSS state; XMM has now observed ~5. Insight into diversity and evolution of novae can be gained by determining when (or if) the SSS stage begins, when turnoff occurs, and how this relates to composition and the mass of the WD. We propose to observe a dozen novae to charaterize their x-ray emission and SSS timescales.

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