X-ray Evolution of Classical Novae: Timescales for the SSS Phase

Details X-ray Evolution of Classical Novae: Timescales for the SSS Phase X-ray Evolution of Classical Novae: Timescales for the SSS Phase

Oct 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005xmm..prop..163s&link_type=abstract

XMM-Newton Proposal ID #04044305

Other

White Dwarf Binaries, Neutron Star Binaries, Cataclysmic Variables, Ulxs, Black Holes, V475 Sct, V574 Pup, V1187 Sco, V5114 Sgr, Yy Dor, Xmm-Newton Proposal 04044305

Scientific paper

The 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 the first year after outburst, and quickly turn off thereafter (the very fast ONeMg novae). Others (e.g., slow novae) are delayed years after outburst before entering the SSS stage, which then lasts many years. ROSAT detected only 3 novae in their SSS state; XMM has observed 5, 3 which have SSS spectrums. Insight into the 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.

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