A Prediction of Supersoft X-Ray Phase of Classical Nova V5583 Sagittarii

TL;DR

This paper predicts the timing of the supersoft X-ray phase of the classical nova V5583 Sagittarii based on optical light curve similarities with a previous nova and theoretical models, guiding future X-ray observations.

Contribution

It introduces a method to estimate the supersoft X-ray phase timing of V5583 Sgr using optical light curve comparison and wind theory models, aiding in targeted observations.

Findings

Optical light curves of V5583 Sgr resemble V382 Vel 1999.

Predicted supersoft X-ray phase between days 100-140 and 200-240 after outburst.

Recommended observation schedule for detecting X-ray phase.

Abstract

We have observed the fast nova V5583 Sagittarii with five B, V, y, R_C, and I_C bands, and found that these multi-band light curves are almost identical with those of V382 Vel 1999 until at least 100 days after outburst. A supersoft X-ray phase of V382 Vel was detected with BeppoSAX about six months after outburst. V5583 Sgr outbursted a few days ago the discovery on 2009 August 6.5 UT near its optical peak. From a complete resemblance between these two nova light curves, we expect a supersoft X-ray phase of V5583 Sgr six months after outburst. Detection of supersoft X-ray turn-on/turnoff dates strongly constrain the evolution of a nova and, as a result, mass range of the WD. For a timely observation of a supersoft X-ray phase of V5583 Sgr, we have calculated nova outburst evolution based on the optically thick wind theory, which predicts the supersoft X-ray phase: it will most probably start between days 100 and 140 and continue until days 200-240 after outburst. We strongly recommend multiple observations during 2009 December, and 2010 January, February, and March to detect the turn-on and turnoff times of the supersoft X-ray phase of V5583 Sgr.