posted on 2018-05-17, 09:13authored byM. 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. C. Horst, R. 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. Vrastil, 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
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.
Funding
We are, as always, grateful to the Swift Team for making the ToO observations possible, in particular to the duty scientists as well as the science planners. This research made use of data supplied by the UK Swift Science Data Centre at the University of Leicester.
Based on observations obtained with XMM-Newton, an ESA science mission with instruments and contributions directly funded by ESA Member States and NASA.
Based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the Data Archive at the Space Telescope Science Institute (STScI), which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. These observations are associated with program #14651. Support for program #14651 was provided by NASA through a grant from STScI.
The Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University (LJMU) in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias with financial support from STFC.
This work makes use of observations from the LCO network.
Based (in part) on data collected with the Danish 1.54m telescope at the ESO La Silla Observatory.
The data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOTSA.
The HET is a joint project of the University of Texas at Austin, the Pennsylvania State University, Stanford University, Ludwig-Maximilians-Universität München, and Georg-August-Universität Göttingen. The HET is named in honor of its principal benefactors, William P. Hobby and Robert E. Eberly.
The LBT is an international collaboration among institutions in the United States, Italy, and Germany. LBT Corporation partners are: The University of Arizona on behalf of the Arizona Board of Regents; Istituto Nazionale di Astrofisica, Italy; LBT Beteiligungsgesellsc
History
Citation
Astrophysical Journal, 2018, 857:68 (29pp)
Author affiliation
/Organisation/COLLEGE OF SCIENCE AND ENGINEERING/Department of Physics and Astronomy