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

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dc.contributor.author Henze, M
dc.contributor.author Darnley, M. J
dc.contributor.author Williams, S. C
dc.contributor.author Kato, M
dc.contributor.author Hachisu, I
dc.contributor.author Anupama, G. C
dc.contributor.author Arai, A
dc.contributor.author Boyd, D
dc.contributor.author Burke, D
dc.contributor.author Ciardullo, R
dc.contributor.author Chinetti, K
dc.contributor.author Cook, L. M
dc.contributor.author Cook, M. J
dc.contributor.author Erdman, P
dc.contributor.author Gao, X
dc.contributor.author Harris, B
dc.contributor.author Hartmann, D. H
dc.contributor.author Hornoch, K
dc.contributor.author Chuck Horst, J
dc.contributor.author Hounsel, R
dc.contributor.author Husar, D
dc.contributor.author Itagaki, K
dc.contributor.author Kabashima, F
dc.contributor.author Kafka, S
dc.contributor.author Kaur, A
dc.contributor.author Kiyota, S
dc.contributor.author Kojiguchi, N
dc.contributor.author Kučáková, H
dc.contributor.author Kuramoto, K
dc.contributor.author Maehara, H
dc.contributor.author Mantero, A
dc.contributor.author Masci, F. J
dc.contributor.author Matsumoto, K
dc.contributor.author Naito, H
dc.contributor.author Ness, J. U
dc.contributor.author Nishiyama, K
dc.contributor.author Oksanen, A
dc.contributor.author Osborne, J. P
dc.contributor.author Page, K. L
dc.contributor.author Paunzen, E
dc.contributor.author Pavana, M
dc.contributor.author Pickard, R
dc.contributor.author Prieto-Arranz, J
dc.contributor.author Rodríguez-Gil, P
dc.contributor.author Sala, G
dc.contributor.author Sano, Y
dc.contributor.author Shafter, A. W
dc.contributor.author Sugiura, Y
dc.contributor.author Tan, H
dc.contributor.author Tordai, T
dc.contributor.author Vraštil, J
dc.contributor.author Wagner, R. M
dc.contributor.author Watanabe, F
dc.contributor.author Williams, B. F
dc.contributor.author Bode, M. F
dc.contributor.author Bruno, A
dc.contributor.author Buchheim, B
dc.contributor.author Crawford, T
dc.contributor.author Goff, B
dc.contributor.author Hernanz, M
dc.contributor.author Igarashi, A. S
dc.contributor.author José, J
dc.contributor.author Motta, M
dc.contributor.author O’Brien, T. J
dc.contributor.author Oswalt, T
dc.contributor.author Poyner, G
dc.contributor.author Ribeiro, V. A. R. M
dc.contributor.author Sabo, R
dc.contributor.author Shara, M.M
dc.contributor.author Shears, J
dc.contributor.author Starkey, D
dc.contributor.author Starrfield, S
dc.contributor.author Woodward, C. E
dc.date.accessioned 2020-11-12T15:00:49Z
dc.date.available 2020-11-12T15:00:49Z
dc.date.issued 2018-04-10
dc.identifier.citation The Astrophysical Journal, Vol. 857, No. 1, 68, pp. 1-29 en_US
dc.identifier.issn 0004-637X
dc.identifier.uri http://prints.iiap.res.in/handle/2248/6942
dc.description Restricted Access © The American Astronomical Society https://doi.org/10.3847/1538-4357/aab6a6 en_US
dc.description.abstract 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. en_US
dc.language.iso en en_US
dc.publisher IOP Publishing en_US
dc.subject Galaxies: individual (M31) en_US
dc.subject novae:Cataclysmic variables en_US
dc.subject Stars: individual (M31N 2008-12a) en_US
dc.subject Ultraviolet: stars en_US
dc.subject X-rays: binaries en_US
dc.title Breaking the Habit: The Peculiar 2016 Eruption of the Unique Recurrent Nova M31N 2008-12a en_US
dc.type Article en_US


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