| 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 |
| URL |
http://adsabs.harvard.edu/abs/2009A%26A...497L...5I |
| 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 |