Discovery of an ∼30-yr-duration post-nova pulsating supersoft source in the Large Magellanic Cloud. Issue 2 (24th September 2020)

• Record Type: Journal Article
• Authors: Vasilopoulos, G; Koliopanos, F; Woods, T E; Haberl, F; Soraisam, M D; Udalski, A
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 499:Issue 2(2020)
• Page Start: 2007
• Page End: 2014
• Publication Date: 2020-09-24
• Subjects: X-rays: binaries -- transients -- stars: white dwarfs -- pulsars: individual: 1RXS J050526.3−684628 -- galaxies: individual: LMC; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/staa2922
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: Supersoft X-ray sources (SSS) have been identified as white dwarfs accreting from binary companions and undergoing nuclear burning of the accreted material on their surface. Although expected to be a relatively numerous population from both binary evolution models and their identification as type Ia supernova progenitor candidates, given the very soft spectrum of SSSs relatively few are known. Here we report on the X-ray and optical properties of 1RXS J050526.3−684628, a previously unidentified accreting nuclear-burning white dwarf located in the Large Magellanic Cloud (LMC). XMM–Newton observations enabled us to study its X-ray spectrum and measure for the first time short-period oscillations of ∼170 s. By analysing newly obtained X-ray data by eROSITA, together with Swift observations and archival ROSAT data, we have followed its long-term evolution over the last 3 decades. We identify 1RXS J050526.3−684628 as a slowly evolving post-nova SSS undergoing residual surface nuclear burning, which finally reached its peak in 2013 and is now declining. Though long expected on theoretical grounds, such long-lived residual-burning objects had not yet been found. By comparison with existing models, we find that the effective temperature and luminosity evolution are consistent with an ∼0.7 M⊙ carbon–oxygen white dwarf accreting ${\sim} 10^{-9}~\rm {M}_{\odot }$ yr −1 . Our results suggest that there may be many more undiscovered SSSs and 'missed' novae awaiting dedicated deep X-ray searches in the LMC and elsewhere.