The short orbital period binary star at the heart of the planetary nebula M 3-1

TL;DR

This paper reports the discovery of the shortest-period binary star at the center of a planetary nebula, providing insights into binary evolution and potential pathways to cataclysmic variables and supernovae.

Contribution

It presents the first detailed analysis of a 3h5m orbital-period binary in a planetary nebula, highlighting its significance for understanding stellar evolution.

Findings

Binary components are close to Roche-lobe-filling.

The system may evolve into a cataclysmic variable.

Potential for nova eruption before nebula dissipates.

Abstract

We present the discovery of a 3h5m orbital-period binary star at the heart of the planetary nebula M 3-1 - the shortest period photometrically-variable central star known and second only to V458 Vul, in general. Combined modelling of light and radial velocity curves reveals both components to be close to Roche-lobe-filling, strongly indicating that the central star will rapidly evolve to become a cataclysmic variable, perhaps experiencing a similar evolution to V458 Vul resulting in a nova eruption before the planetary nebula has fully dissipated. While the short orbital period and near Roche-lobe filling natures of both components make the central binary of M 3-1 an important test case with which to constrain the formation processes of cataclysmic variables, novae and perhaps even supernovae type Ia.