Einstein Probe discovery of EP J005245.1-722843: a rare BeWD binary in the Small Magellanic Cloud?

TL;DR

The Einstein Probe detected a rare super-soft X-ray outburst in the Small Magellanic Cloud, revealing a likely Be white dwarf binary system with a massive, near-Chandrasekhar limit white dwarf, providing insights into this elusive evolutionary stage.

Contribution

This is the first detection of a super-soft outburst from a Be white dwarf binary in the SMC, suggesting a new class of accreting white dwarf systems and their evolutionary pathways.

Findings

Detected a super-soft X-ray outburst with a very short duration.

Identified spectral features indicating a massive Ne-O white dwarf.

Suggested the system is a Be white dwarf binary near the Chandrasekhar limit.

Abstract

On May 27 2024, the Wide-field X-ray Telescope onboard the Einstein Probe (EP) mission detected enhanced X-ray emission from a new transient source in the Small Magellanic Cloud (SMC) during its commissioning phase. Prompt follow-up with the EP Follow-up X-ray Telescope, the Swift X-ray Telescope and NICER have revealed a very soft, thermally emitting source (kT$\sim$0.1 keV at the outburst peak) with an X-ray luminosity of $L\sim4\times10^{38}$ erg s$^{-1}$, labelled EP J005245.1-722843. This super-soft outburst faded very quickly in a week time. Several emission lines and absorption edges were present in the X-ray spectrum, including deep Nitrogen (0.67 keV) and Oxygen (0.87 keV) absorption edges. The X-ray emission resembles the SSS phase of typical nova outbursts from an accreting white dwarf (WD) in a binary system, despite the X-ray source being historically associated with an O9-B0e massive star exhibiting a 17.55 days periodicity in the optical band. The discovery of this super-soft outburst suggests that EP J005245.1-722843 is a BeWD X-ray binary: an elusive evolutionary stage where two main-sequence massive stars have undergone a common envelope phase and experienced at least two episodes of mass transfer. In addition, the very short duration of the outburst and the presence of Ne features hint at a rather massive, i.e., close to the Chandrasekhar limit, Ne-O WD in the system.