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 |
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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 |
|