GW Librae: A unique laboratory for pulsations in an accreting white dwarf

TL;DR

This study investigates the pulsation behavior of the accreting white dwarf GW Librae through ultraviolet spectroscopy, revealing temperature variations and unusual long-term variability linked to pulsations and stellar rotation.

Contribution

The paper provides new ultraviolet observations of GW Librae, demonstrating temperature variations associated with pulsations and identifying a novel long-term variability pattern.

Findings

Pulsations cause temperature variations consistent with theoretical predictions.

Detected high-amplitude ~4.4h variability not previously observed.

Temperature increase in a large surface region is linked to pulsation activity.

Abstract

Non-radial pulsations have been identified in a number of accreting white dwarfs in cataclysmic variables. These stars offer insight into the excitation of pulsation modes in atmospheres with mixed compositions of hydrogen, helium, and metals, and the response of these modes to changes in the white dwarf temperature. Among all pulsating cataclysmic variable white dwarfs, GW Librae stands out by having a well-established observational record of three independent pulsation modes that disappeared when the white dwarf temperature rose dramatically following its 2007 accretion outburst. Our analysis of HST ultraviolet spectroscopy taken in 2002, 2010 and 2011, showed that pulsations produce variations in the white dwarf effective temperature as predicted by theory. Additionally in May~2013, we obtained new HST/COS ultraviolet observations that displayed unexpected behaviour: besides showing variability at ~275s, which is close to the post-outburst pulsations detected with HST in 2010 and 2011, the white dwarf exhibits high-amplitude variability on a ~4.4h time-scale. We demonstrate that this variability is produced by an increase of the temperature of a region on white dwarf covering up to ~30 per cent of the visible white dwarf surface. We argue against a short-lived accretion episode as the explanation of such heating, and discuss this event in the context of non-radial pulsations on a rapidly rotating star