Breaking the habit - the peculiar 2016 eruption of the unique recurrent nova M31N 2008-12a

TL;DR

The 2016 eruption of the recurrent nova M31N 2008-12a was peculiar, showing delays and a shorter supersoft X-ray phase, likely caused by a lower accretion rate affecting eruption properties.

Contribution

This study documents the unusual 2016 eruption of M31N 2008-12a and interprets it through theoretical models linking accretion rate variations to eruption characteristics.

Findings

2016 eruption showed delayed onset and shorter SSS phase.

Optical peak was brighter with a cusp shape.

Models suggest lower accretion rate caused these differences.

Abstract

Since its discovery in 2008, the Andromeda galaxy nova M31N 2008-12a has been observed in eruption every single year. This unprecedented frequency indicates an extreme object, with a massive white dwarf and a high accretion rate, which is the most promising candidate for the single-degenerate progenitor of a type-Ia supernova known to date. The previous three eruptions of M31N 2008-12a have displayed remarkably homogeneous multi-wavelength properties: (i) From a faint peak, the optical light curve declined rapidly by two magnitudes in less than two days; (ii) Early spectra showed initial high velocities that slowed down significantly within days and displayed clear He/N lines throughout; (iii) The supersoft X-ray source (SSS) phase of the nova began extremely early, six days after eruption, and only lasted for about two weeks. In contrast, the peculiar 2016 eruption was clearly different. Here we report (i) the considerable delay in the 2016 eruption date, (ii) the significantly shorter SSS phase, and (iii) the brighter optical peak magnitude (with a hitherto unobserved cusp shape). Early theoretical models suggest that these three different effects can be consistently understood as caused by a lower quiescence mass-accretion rate. The corresponding higher ignition mass caused a brighter peak in the free-free emission model. The less-massive accretion disk experienced greater disruption, consequently delaying re-establishment of effective accretion. Without the early refueling, the SSS phase was shortened. Observing the next few eruptions will determine whether the properties of the 2016 outburst make it a genuine outlier in the evolution of M31N 2008-12a.