Lessons from the Onset of a Common Envelope Episode: the Remarkable M31 2015 Luminous Red Nova Outburst

TL;DR

This study analyzes the 2015 luminous red nova in Andromeda, revealing details of the common envelope phase and stellar merger process through photometry, spectroscopy, and modeling.

Contribution

It provides the first detailed observational constraints on the early stages of a common envelope episode in a stellar merger.

Findings

The transient involved two ejecta components with different masses.

The primary star was a 3-5.5 solar mass sub-giant expanding before merger.

The merger likely involved a low-mass companion of 0.1-0.6 solar masses.

Abstract

This paper investigates the recent stellar merger transient M31LRN 2015 in the Andromeda galaxy. We analyze published optical photometry and spectroscopy along with a Hubble Space Telescope detection of the color and magnitude of the pre-outburst source. The transient outburst is consistent with dynamically driven ejecta at the onset of a common envelope episode, which eventually leads to the complete merger of a binary system. The light curve appears to contain two components: first $\sim10^{-2} M_\odot$ of fast ejecta driven by shocks at the onset of common envelope, and later, $\sim0.3 M_\odot$ of further ejecta as the secondary becomes more deeply engulfed within the primary. Just prior to merger, we find that the primary star is a $3-5.5 M_\odot$ sub-giant branch primary star with radius of $30-40R_\odot$. Its position in the color-magnitude diagram shows that it is growing in radius, consistent with a picture where it engulfs its companion. By matching the properties of the primary star to the transient outburst, we show that the optical transient lasts less than ten orbits of the original binary, which had a pre-merger period of $\sim 10$ days. We consider the possible orbital dynamics leading up to the merger, and argue that if the system merged due to the Darwin tidal instability it implies a lower mass main sequence companion of $0.1-0.6M_\odot$. This analysis represents a promising step toward a more detailed understanding of flows in common envelope episodes through direct observational constraints.