Orbital periods of cataclysmic variables identified by the SDSS. VIII. A slingshot prominence in SDSS J003941.06+005427.5?

TL;DR

This study investigates a faint cataclysmic variable, revealing a unique emission feature likely caused by a coronal loop, suggesting a possible first observation of a slingshot prominence in such systems.

Contribution

The paper reports the discovery of a potential slingshot prominence in a low mass-transfer rate cataclysmic variable, a novel observation in this class of binary systems.

Findings

Orbital period of 91.395 minutes measured from H-alpha emission.

Detection of a third emission peak possibly due to a coronal loop.

Indication that SDSS J003941.06+005427.5 may be a post-bounce CV.

Abstract

We present VLT spectroscopy and NTT photometry of the faint cataclysmic binary SDSS J003941.06+005427.5. This object shows triple-peaked H-alpha emission with all three peaks variable in both strength and velocity. We measure an orbital period of 91.395 +/- 0.093 min from the velocity variations of the wings of the H-alpha emission line. Using the GALEX and SDSS photometry of this object, we determine a white dwarf temperature of 15000 K and a very late (>=L2) spectral type for the companion star. These measurements, plus the relatively long orbital period, suggest that SDSS J003941.06+005427.5 may be a post-bounce cataclysmic variable. Doppler maps of the H-alpha and He I 6678A emission features show an accretion disc with a non-uniform brightness and departures from Keplerian flow. The third emission peak is detected only in H-alpha and at a relatively low velocity amplitude of 202 +/- 3 km/s. We are unable to explain this emission as arising from either the white dwarf, the secondary star, or the accretion disc. We tentatively attribute this mysterious central peak to a coronal loop anchored at the secondary star. If confirmed, this would be the first example of a slingshot prominence in a CV with a low mass-transfer rate and/or a fully convective secondary star.