A Prediction Formula of Supersoft X-ray Phase of Classical Novae

TL;DR

This paper develops prediction formulas for the supersoft X-ray phases of classical novae based on a universal decline law, and estimates white dwarf masses by fitting models to observed optical and X-ray data.

Contribution

It introduces new predictive formulas for X-ray on/off times and provides theoretical MMRD relations considering WD mass and envelope mass, aligning with empirical data.

Findings

Predicted X-ray on and off times based on t_3 decline parameter.

Estimated WD masses for ten novae using combined optical and X-ray data.

Established theoretical MMRD relations consistent with empirical formulas.

Abstract

On the basis of the recently developed universal decline law of classical novae, we propose prediction formulae for supersoft X-ray on and off times, i.e., t_{X-on} = (10 \pm 1.8) t_3 days and t_{X-off} = (5.3 \pm 1.4) (t_3)^{1.5} days for 8 < t_3 < 80 days. We have determined the absolute magnitude of our free-free emission model light curves and derived maximum magnitude vs. rate of decline (MMRD) relations. Our theoretical MMRD relations are governed by two parameters, one is the white dwarf (WD) mass and the other is the initial envelope mass at a nova outburst; this second parameter explains the scatter of MMRD points of individual novae. Our theoretical MMRD relations are also in good agreement with the well-known empirical formulae. We also show another empirical relation of M_V(15) ~ -5.7 \pm 0.3 based on the absolute magnitude of our model light curves, i.e., the absolute magnitude at 15 days after optical maximum is almost common among various novae. We analyzed ten nova light curves, in which a supersoft X-ray phase was detected, and estimated their WD masses. The models best reproducing simultaneously the optical and supersoft X-ray observations are ONeMg WDs with 1.28 \pm 0.04 M_\sun (V598 Pup), 1.23 \pm 0.05 M_\sun (V382 Vel), 1.15 \pm 0.06 M_\sun (V4743 Sgr), 1.13 \pm 0.06 M_\sun (V1281 Sco), 1.2 \pm 0.05 M_\sun (V597 Pup), 1.06 \pm 0.07 M_\sun (V1494 Aql), 1.04 \pm 0.07 M_\sun (V2467 Cyg), 1.07 \pm 0.07 M_\sun (V5116 Sgr), 1.05 \pm 0.05 M_\sun (V574 Pup), and a CO WD with 0.93 \pm 0.08 M_\sun (V458 Vul). The newly proposed relationships are consistent with the emergence or decay epoch of the supersoft X-ray phase of these ten novae. Finally, we discuss the mechanism of shock-origin hard X-ray component in relation to the emergence of companion star from the WD envelope.