Population of post-nova supersoft X-ray sources

TL;DR

This study models the expected population of post-nova supersoft X-ray sources in M31, predicting their numbers, luminosities, and temperatures, and compares these predictions with XMM-Newton observations to assess model accuracy.

Contribution

It provides the first comprehensive population estimates of post-nova supersoft X-ray sources in M31 using evolutionary models and compares predictions with observational data.

Findings

Predicted 250-600 post-nova SSSs in M31 at any time.

Predicted combined luminosity of ~10^39 erg/s.

Predicted number exceeds observed by a factor of 2-5, but aligns with uncertainties.

Abstract

Novae undergo a supersoft X-ray phase of varying duration after the optical outburst. Such transient post-nova supersoft X-ray sources (SSSs) are the majority of the observed SSSs in M31. In this paper, we use the post-nova evolutionary models of Wolf et al. to compute the expected population of post-nova SSSs in M31. We predict that depending on the assumptions about the WD mass distribution in novae, at any instant there are about 250-600 post-nova SSSs in M31 with (unabsorbed) 0.2-1.0 keV luminosity L_x>10^36 erg/s. Their combined unabsorbed luminosity is of the order of ~10^39 erg/s. Their luminosity distribution shows significant steepening around log(L_x)~37.7-38 and becomes zero at L_x~2x10^38 erg/s, the maximum L_x achieved in the post-nova evolutionary tracks. Their effective temperature distribution has a roughly power law shape with differential slope of ~4-6 up to the maximum temperature of T_eff~1.5x10^6 K. We compare our predictions with the results of the XMM-Newton monitoring of the central field of M31 between 2006 and 2009. The predicted number of post-nova SSSs exceed the observed number by a factor of ~2-5, depending on the assumed WD mass distribution in novae. This is good agreement, considering the number and magnitude of uncertainties involved in calculations of the post-nova evolutionary models and their X-ray output. Furthermore, only a moderate circumstellar absorption, with hydrogen column density of the order of ~10^21 cm^-2, will remove the discrepancy.