Breaking the Habit: The Peculiar 2016 Eruption of the Unique Recurrent Nova M31N 2008-12a

M. Henze, M. Henze, M. J. Darnley, S. C. Williams, M. Kato, I. Hachisu, G. C. Anupama, A. Arai, D. Boyd, D. Burke, R. Ciardullo, K. Chinetti, L. M. Cook, M. J. Cook, P. Erdman, X. Gao, B. Harris, D. H. Hartmann, K. Hornoch, J. Chuck HorstR. Hounsell, D. Husar, K. Itagaki, F. Kabashima, S. Kafka, A. Kaur, S. Kiyota, N. Kojiguchi, H. Kučáková, K. Kuramoto, H. Maehara, A. Mantero, F. J. Masci, K. Matsumoto, H. Naito, J. U. Ness, K. Nishiyama, A. Oksanen, J. P. Osborne, K. L. Page, E. Paunzen, M. Pavana, R. Pickard, J. Prieto-Arranz, P. Rodríguez-Gil, G. Sala, Y. Sano, A. W. Shafter, Y. Sugiura, H. Tan, T. Tordai, J. Vraštil, R. M. Wagner, F. Watanabe, B. F. Williams, M. F. Bode, A. Bruno, B. Buchheim, T. Crawford, B. Goff, M. Hernanz, A. S. Igarashi, J. José, M. Motta, T. J. O'Brien, T. Oswalt, G. Poyner, V. A.R.M. Ribeiro, R. Sabo, M. M. Shara, J. Shears, D. Starkey, S. Starrfield, C. E. Woodward

Research output: Contribution to journalArticlepeer-review

12 Scopus citations

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 multiwavelength 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, and (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 the 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.

Original languageEnglish (US)
Article number68
JournalAstrophysical Journal
Volume857
Issue number1
DOIs
StatePublished - Apr 10 2018

Bibliographical note

Funding Information:
IRAF is distributed by the National Optical Astronomy Observatory, which is operated by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation.

Funding Information:
The Institute for Gravitation and the Cosmos is supported by the Eberly College of Science and the Office of the Senior Vice President for Research at the Pennsylvania State University.

Funding Information:
K. L.P. and J.P.O. acknowledge the support of the UK Space Agency.

Funding Information:
S.S. acknowledges partial support to ASU from NASA and HST grants.

Keywords

  • X-rays: binaries
  • galaxies: individual (M31)
  • novae, cataclysmic variables
  • stars: individual (M31N 2008-12a)
  • ultraviolet: stars

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