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arXiv · 0909.1670

X-ray and UV observations of nova V598 Puppis between 147 and 255 days after outburst

K. L. Page·J. P. Osborne·A. M. Read·P. A. Evans·J. -U. Ness·A. P. Beardmore·M. Bode·G. J. Schwarz·S. Starrfield
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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 ~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(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 ~ 2246-2600 angstrom) between days 169 and 255.

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K. L. Page, J. P. Osborne, A. M. Read, P. A. Evans, J. -U. Ness, A. P. Beardmore, M. Bode, G. J. Schwarz, S. Starrfield. 2009-09-09. X-ray and UV observations of nova V598 Puppis between 147 and 255 days after outburst. https://doi.org/10.1051/0004-6361/200912985

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