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

Type Journal Article
Names A. Ibarra, E. Kuulkers, J. P. Osborne, K. Page, J. U. Ness, R. D. Saxton, W. Baumgartner, V. Beckmann, M. F. Bode, M. Hernanz, K. Mukai, M. Orio, G. Sala, S. Starrfield, G. A. Wynn
Publication Astronomy and Astrophysics
Volume 497
Issue 1
Pages L5-L8
Date April 1, 2009
Library Catalog NASA ADS
Abstract Classical novae are phenomena caused by explosive hydrogen burning onto an accreting white dwarf. Only one classical nova had 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 to date. 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 exhibits a soft X-ray source.
Tags Cataclysmic Variables, NOVAE, X-Rays: Binaries
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