Detection of accretion X-rays from QS Vir: cataclysmic or a lot of hot air?

TL;DR

This study detects X-ray eclipses in QS Vir indicating low-rate accretion onto its white dwarf, likely driven by chromospheric flows rather than wind or Roche lobe overflow, suggesting a rare evolutionary phase.

Contribution

First X-ray detection of accretion in QS Vir, revealing a low accretion rate and proposing a novel accretion mechanism involving chromospheric flows.

Findings

X-ray eclipses confirm mass transfer onto white dwarf

Accretion rate is among the lowest for non-magnetic systems

Chromospheric flows may supplement Roche lobe overflow

Abstract

An XMM-Newton observation of the nearby "pre-cataclysmic" short-period (P_orb = 3.62 hr) binary QS Vir (EC 13471-1258) revealed regular narrow X-ray eclipses when the white dwarf passed behind its M2-4 dwarf companion. The X-ray emission provides a clear signature of mass transfer and accretion onto the white dwarf. The low-resolution XMM-Newton EPIC spectra are consistent with a cooling flow model and indicate an accretion rate of Mdot= 1.7\times10^-13M\odot/yr. At 48 pc distant, QS Vir is then the second nearest accreting cataclysmic variable known, with one of the lowest accretion rates found to date for a non-magnetic system. To feed this accretion through a wind would require a wind mass loss rate of Mdot ~ 2 \times 10^-12M\odot/yr if the accretion efficiency is of the order of 10%. Consideration of likely mass loss rates for M dwarfs suggests this is improbably high and pure wind accretion unlikely. A lack of accretion disk signatures also presents some difficulties for direct Roche lobe overflow. We speculate that QS Vir is on the verge of Roche lobe overflow, and that the observed mass transfer could be supplemented by upward chromospheric flows on the M dwarf, analogous to spicules and mottles on the Sun, that escape the Roche surface to be subsequently swept up into the white dwarf Roche lobe. If so, QS Vir would be in a rare evolutionary phase lasting only a million years. The X-ray luminosity of the M dwarf estimated during primary eclipse is L_X = 3 \times 10^28 erg/s, which is consistent with that of rapidly rotating "saturated" K and M dwarfs.