Facial reconstruction

Search LJMU Research Online

Browse Repository | Browse E-Theses

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

Henze, M, Darnley, MJ, Williams, SC, Kato, M, Hachisu, I, Anupama, GC, Arai, A, Boyd, D, Burke, D, Chinetti, K, Ciardullo, R, Cook, LM, Cook, MJ, Erdman, P, Gao, X, Harris, B, Hartmann, DH, Hornoch, K, Horst, JC, Hounsell, R , Husar, D, Itagaki, K, Kabashima, F, Kafka, S, Kaur, A, Kiyota, S, Kojiguchi, N, Kucakova, H, Kuramoto, K, Maehara, H, Mantero, A, Masci, FJ, Matsumoto, K, Naito, H, Ness, J-U, Nishiyama, K, Oksanen, A, Osborne, JP, Page, KL, Paunzen, E, Pavana, M, Pickard, R, Prieto-Arranz, J, Rodriguez-Gil, P, Sala, G, Sano, Y, Shafter, AW, Sugiura, Y, Tan, H, Tordai, T, Vratil, J, Wagner, RM, Watanabe, F, Williams, BF, Bode, MF, Bruno, A, Buchheim, B, Crawford, T, Goff, B, Hernanz, M, Igarashi, AS, Jose, J, Motta, M, O'Brien, TJ, Oswalt, T, Poyner, G, Ribeiro, VARM, Sabo, R, Shara, MM, Shears, J, Starkey, D, Starrfield, S and Woodward, CE Breaking the habit - the peculiar 2016 eruption of the unique recurrent nova M31N 2008-12a. The Astrophysical Journal. ISSN 1538-4357 (Accepted)

1803.00181v1.pdf - Accepted Version

Download (1MB) | Preview


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.

Item Type: Article
Uncontrolled Keywords: astro-ph.SR; astro-ph.SR; astro-ph.HE
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Divisions: Astrophysics Research Institute
Publisher: American Astronomical Society
Related URLs:
Date Deposited: 05 Mar 2018 09:29
Last Modified: 05 Mar 2018 09:29
URI: http://researchonline.ljmu.ac.uk/id/eprint/8173

Actions (login required)

View Item View Item