Pre-nova X-ray observations of V2491 Cyg (Nova Cyg 2008b)

Details Pre-nova X-ray observations of V2491 Cyg (Nova Cyg 2008b) Pre-nova X-ray observations of V2491 Cyg (Nova Cyg 2008b)

2009-02-23

arxiv.org/abs/0902.3943v1

Astronomy and Astrophysics

Astrophysics

Galaxy Astrophysics

4 pages, 2 figures. Astronomy and Astrophysics, in press

Scientific paper

10.1051/0004-6361/200911710

Classical novae are phenomena caused by explosive hydrogen burning on an accreting white dwarf. So far, only one classical nova has been identified in X-rays before the actual optical outburst occurred (V2487 Oph). The recently discovered nova, V2491 Cyg, is one of the fastest (He/N) novae observed so far. Using archival ROSAT, XMM-Newton and Swift data, we show that V2491 Cyg was a persistent X-ray source during its quiescent time before the optical outburst. We present the X-ray spectral characteristics and derive X-ray fluxes. The pre-outburst X-ray emission is variable, and at least in one observation it shows a very soft X-ray source.

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