Volume 507, Number 2, November IV 2009
|Page(s)||923 - 927|
|Section||Stellar structure and evolution|
|Published online||15 September 2009|
X-ray and UV observations of nova V598 Puppis between 147 and 255 days after outburst
Dept. of Physics and Astronomy, University of Leicester, Leicester, LE1 7RH, UK e-mail: email@example.com
2 XMM-Newton Science Operations Centre, ESAC, Apartado 78, 28691 Villanueva de la Cañada, Madrid, Spain
3 Astrophysics Research Institute, Liverpool John Moores University, Birkenhead, CH41 1LD, UK
4 Department of Geology and Astronomy, West Chester University, West Chester, PA 19383, USA
5 School of Earth and Space Exploration, Arizona State University, Tempe, AZ 85287-1404, USA
Accepted: 8 September 2009
Aims. The launch of Swift has allowed many more novae to be observed regularly over the X-ray band. Such X-ray observations of novae can reveal ejecta shocks and the nuclear burning white dwarf, allowing estimates to be made of the ejecta velocity.
Methods. We analyse XMM-Newton and Swift X-ray and UV observations of the nova V598 Pup, which was initially discovered in the XMM-Newton slew survey. These data were obtained between 147 and 255 days after the nova outburst, and are compared with the earlier, brighter slew detection.
Results. The X-ray spectrum consists of a super-soft source, with the soft emission becoming hotter and much fainter between days ~147 and ~172 after the outburst, and a more slowly declining optically thin component, formed by shocks with –800 eV (corresponding to velocities of 400–800 km s-1). The main super-soft phase had a duration of less than 130 days. The Reflection Grating Spectrometer data show evidence of emission lines consistent with optically thin emission of eV and place a limit on the density of the surrounding medium of log (ne/cm-3) < 10.4 at the 90% level. The UV emission is variable over short timescales and fades by at least one magnitude (at λ ~ 2246–2600 Å) between days 169 and 255.
Key words: stars: individual: V598 Pup / stars: novae, cataclysmic variables
© ESO, 2009
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