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 kT ∼ 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 ∼ 100 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.
- Stars: individual: V598 Pup
- Stars: novae, cataclysmic variables
ASJC Scopus subject areas
- Astronomy and Astrophysics
- Space and Planetary Science