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

TL;DR

This study analyzes X-ray and UV observations of nova V598 Puppis over 147 to 255 days post-outburst, revealing details about ejecta shocks, the super-soft phase, and UV variability, contributing to understanding nova evolution.

Contribution

First detailed X-ray and UV analysis of V598 Puppis over this period, providing insights into shock velocities, super-soft phase duration, and surrounding medium density.

Findings

Super-soft source lasted less than 130 days.

Ejecta shock velocities estimated at 400-800 km/s.

UV emission faded by at least one magnitude.

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.