X-ray and optical observations of the unique binary system HD49798/RXJ0648.0-4418

TL;DR

This study presents detailed X-ray and optical observations of the unique binary system HD49798/RXJ0648.0-4418, revealing its composition, accretion processes, and potential as a supernova progenitor or millisecond pulsar formation site.

Contribution

First comprehensive X-ray detection of a hot sub-dwarf star in a binary system with a white dwarf, including insights into accretion and evolutionary future.

Findings

White dwarf has a rapid 13.2 s rotation period and a mass of 1.28 M_sun.

X-ray emission includes a soft blackbody component and a faint hard power-law component.

Potential evolution into a millisecond pulsar or Type Ia supernova progenitor.

Abstract

We report the results of XMM-Newton observations of HD49798/RXJ0648.0-4418, the only known X-ray binary consisting of a hot sub-dwarf and a white dwarf. The white dwarf rotates very rapidly (P=13.2 s) and has a dynamically measured mass of 1.28+/-0.05 M_sun. Its X-ray emission consists of a strongly pulsed, soft component, well fit by a blackbody with kT~40 eV, accounting for most of the luminosity, and a fainter hard power-law component (photon index ~1.6). A luminosity of ~10^{32} erg/s is produced by accretion onto the white dwarf of the helium-rich matter from the wind of the companion, which is one of the few hot sub-dwarfs showing evidence of mass-loss. A search for optical pulsations at the South African Astronomical Observatory 1.9-m telescope gave negative results. X-rays were detected also during the white dwarf eclipse. This emission, with luminosity 2x10^{30} erg/s, can be attributed to HD 49798 and represents the first detection of a hot sub-dwarf star in the X-ray band. HD49798/RXJ0648.0-4418 is a post-common envelope binary which most likely originated from a pair of stars with masses ~8-10 M_sun. After the current He-burning phase, HD 49798 will expand and reach the Roche-lobe, causing a higher accretion rate onto the white dwarf which can reach the Chandrasekhar limit. Considering the fast spin of the white dwarf, this could lead to the formation of a millisecond pulsar. Alternatively, this system could be a Type Ia supernova progenitor with the appealing characteristic of a short time delay, being the descendent of relatively massive stars.