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dc.contributor.author | Darnley M. | |
dc.contributor.author | Henze M. | |
dc.contributor.author | Bode M. | |
dc.contributor.author | Hachisu I. | |
dc.contributor.author | Hernanz M. | |
dc.contributor.author | Hornoch K. | |
dc.contributor.author | Hounsell R. | |
dc.contributor.author | Kato M. | |
dc.contributor.author | Ness J. | |
dc.contributor.author | Osborne J. | |
dc.contributor.author | Page K. | |
dc.contributor.author | Ribeiro V. | |
dc.contributor.author | Rodríguez-Gil P. | |
dc.contributor.author | Shafter A. | |
dc.contributor.author | Shara M. | |
dc.contributor.author | Steele I. | |
dc.contributor.author | Williams S. | |
dc.contributor.author | Arai A. | |
dc.contributor.author | Arcavi I. | |
dc.contributor.author | Barsukova E. | |
dc.contributor.author | Boumis P. | |
dc.contributor.author | Chen T. | |
dc.contributor.author | Fabrika S. | |
dc.contributor.author | Figueira J. | |
dc.contributor.author | Gao X. | |
dc.contributor.author | Gehrels N. | |
dc.contributor.author | Godon P. | |
dc.contributor.author | Goranskij V. | |
dc.contributor.author | Harman D. | |
dc.contributor.author | Hartmann D. | |
dc.contributor.author | Hosseinzadeh G. | |
dc.contributor.author | Horst J. | |
dc.contributor.author | Itagaki K. | |
dc.contributor.author | José J. | |
dc.contributor.author | Kabashima F. | |
dc.contributor.author | Kaur A. | |
dc.contributor.author | Kawai N. | |
dc.contributor.author | Kennea J. | |
dc.contributor.author | Kiyota S. | |
dc.contributor.author | Kučáková H. | |
dc.contributor.author | Lau K. | |
dc.contributor.author | Maehara H. | |
dc.contributor.author | Naito H. | |
dc.contributor.author | Nakajima K. | |
dc.contributor.author | Nishiyama K. | |
dc.contributor.author | O'Brien T. | |
dc.contributor.author | Quimby R. | |
dc.contributor.author | Sala G. | |
dc.contributor.author | Sano Y. | |
dc.contributor.author | Sion E. | |
dc.contributor.author | Valeev A. | |
dc.contributor.author | Watanabe F. | |
dc.contributor.author | Watanabe M. | |
dc.contributor.author | Williams B. | |
dc.contributor.author | Xu Z. | |
dc.date.accessioned | 2018-09-19T20:06:22Z | |
dc.date.available | 2018-09-19T20:06:22Z | |
dc.date.issued | 2016 | |
dc.identifier.issn | 0004-637X | |
dc.identifier.uri | https://dspace.kpfu.ru/xmlui/handle/net/142562 | |
dc.description.abstract | © 2016. The American Astronomical Society. All rights reserved.The Andromeda Galaxy recurrent nova M31N 2008-12a had been observed in eruption 10 times, including yearly eruptions from 2008 to 2014. With a measured recurrence period of Prec = 351 ± 13 days (we believe the true value to be half of this) and a white dwarf very close to the Chandrasekhar limit, M31N 2008-12a has become the leading pre-explosion supernova type Ia progenitor candidate. Following multi-wavelength follow-up observations of the 2013 and 2014 eruptions, we initiated a campaign to ensure early detection of the predicted 2015 eruption, which triggered ambitious ground- and space-based follow-up programs. In this paper we present the 2015 detection, visible to near-infrared photometry and visible spectroscopy, and ultraviolet and X-ray observations from the Swift observatory. The LCOGT 2 m (Hawaii) discovered the 2015 eruption, estimated to have commenced at August 28.28 ± 0.12 UT. The 2013-2015 eruptions are remarkably similar at all wavelengths. New early spectroscopic observations reveal short-lived emission from material with velocities ∼13,000 km s-1, possibly collimated outflows. Photometric and spectroscopic observations of the eruption provide strong evidence supporting a red giant donor. An apparently stochastic variability during the early supersoft X-ray phase was comparable in amplitude and duration to past eruptions, but the 2013 and 2015 eruptions show evidence of a brief flux dip during this phase. The multi-eruption Swift/XRT spectra show tentative evidence of high-ionization emission lines above a high-temperature continuum. Following Henze et al. (2015a), the updated recurrence period based on all known eruptions is Prec = 174 ± 10 days, and we expect the next eruption of M31N 2008-12a to occur around 2016 mid-September. | |
dc.relation.ispartofseries | Astrophysical Journal | |
dc.subject | galaxies: individual (M31) | |
dc.subject | novae, cataclysmic variables | |
dc.subject | stars: individual (M31N 2008-12a) | |
dc.subject | ultraviolet: stars | |
dc.subject | X-rays: binaries | |
dc.title | M31N 2008-12a - The REMARKABLE RECURRENT NOVA in M31: PANCHROMATIC OBSERVATIONS of the 2015 ERUPTION | |
dc.type | Article | |
dc.relation.ispartofseries-issue | 2 | |
dc.relation.ispartofseries-volume | 833 | |
dc.collection | Публикации сотрудников КФУ | |
dc.source.id | SCOPUS0004637X-2016-833-2-SID85007524590 |