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- W1906221824 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 white dwarf (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 Lx ≥ 1036 erg s−1. Their combined unabsorbed luminosity is of the order of ∼1039 erg s−1. Their luminosity distribution shows significant steepening around log (Lx) ∼ 37.7–38 and becomes zero at Lx ≈ 2 × 1038 erg s−1, the maximum Lx 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 Teff ≈ 1.5 × 106 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 exceeds 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 ∼1021 cm−2, will remove the discrepancy." @default.
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- W1906221824 date "2015-11-05" @default.
- W1906221824 modified "2023-10-07" @default.
- W1906221824 title "Population of post-nova supersoft X-ray sources" @default.
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- W1906221824 doi "https://doi.org/10.1093/mnras/stv2359" @default.
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