X-ray and UV observations of nova V598 Puppis between 147 and 255 days after outburst
ASTRONOMY & ASTROPHYSICS(2009)
Abstract
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 similar to 147 and similar to 172 after the outburst, and a more slowly declining optically thin component, formed by shocks with kT similar to 200-800 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 kT similar to 100 eV and place a limit on the density of the surrounding medium of log (n(e)/cm(-3)) < 10.4 at the 90% level. The UV emission is variable over short timescales and fades by at least one magnitude (at lambda similar to 2246-2600 angstrom) between days 169 and 255.
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Key words
stars: individual: V598 Pup,stars: novae, cataclysmic variables
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