M31N 2008-12a-THE REMARKABLE RECURRENT NOVA IN M31: PANCHROMATIC OBSERVATIONS OF THE 2015 ERUPTION

被引：46

作者：

Darnley, M. J. ^{[1
]}

Henze, M. ^{[2
]}

Bode, M. F. ^{[1
]}

Haciusu, I. ^{[3
]}

Hernanz, M. ^{[2
]}

Hornoch, K. ^{[4
]}

Hounsell, R. ^{[5
]}

Kato, M. ^{[6
]}

Ness, J. -U. ^{[7
]}

Osborne, J. P. ^{[8
]}

Page, K. L. ^{[8
]}

Ribeiro, V. A. R. M. ^{[9
]}

Rodriguez-Gil, P. ^{[10
,11
]}

Shafter, A. W. ^{[12
]}

Shara, M. M. ^{[13
]}

Steele, I. A. ^{[1
]}

Williams, S. C. ^{[1
,14
]}

Arai, A. ^{[15
]}

Arcavi, I. ^{[16
]}

Barsukova, E. A. ^{[17
]}

Boumis, P. ^{[19
]}

Chen, T. ^{[20
]}

Fabrika, S. ^{[18
,21
]}

Figueira, J. ^{[22
,23
]}

Gao, X. ^{[24
]}

Gehrels, N. ^{[25
]}

Godon, P. ^{[26
]}

Goranskij, V. P. . ^{[27
]}

Harman, D. J. ^{[1
]}

Hartmann, D. H. ^{[28
]}

Hosseinzade, G. ^{[16
,29
]}

Horst, J. Chuck ^{[12
]}

Itagam, K. ^{[30
]}

Jose, J. ^{[22
,23
]}

Kabashima, F. ^{[31
]}

Kaur, A. ^{[28
]}

Kawm, N. ^{[32
]}

Kennea, J. A. ^{[33
]}

Kiyota, S. ^{[34
]}

Kucakkova, H. ^{[35
]}

Lau, K. M. ^{[20
]}

Maehara, H. ^{[36
]}

Naito, H. ^{[37
]}

Nakajima, K. ^{[37
,38
]}

Nishiyama, K. ^{[31
]}

O'Brien, T. J. ^{[39
]}

Quimby, R. ^{[12
]}

Sala, G. ^{[22
,23
]}

Sano, Y. ^{[37
,40
]}

Sion, E. M. ^{[26
]}

机构：

[1] Liverpool John Moores Univ, Astrophys Res Inst, IC2 Liverpool Sci Pk, Liverpool L3 5RF, Merseyside, England

[2] CSIC IEEC, Inst Ciencies Espai, Campus UAB,C Can Magrans S-N, E-08193 Cerdanyola Del Valles, Spain

[3] Univ Tokyo, Dept Earth Sci & Astron, Coll Arts & Sci, Meguro Ku, 3-8-1 Komaba, Tokyo 1538902, Japan

[4] Acad Sci, Astron Inst, CZ-25165 Ondrejov, Czech Republic

[5] Univ Illinois, Dept Astron, 1002 W Green St, Urbana, IL 61801 USA

[6] Keio Univ, Dept Astron, Yokohama, Kanagawa 2238521, Japan

[7] European Space Astron Ctr, Camino Bajo Castillo S-N, E-28692 Madrid, Spain

[8] Univ Leicester, Dept Phys & Astron, Xray & Observat Astron Grp, Leicester LE1 7RH, Leics, England

[9] Radboud Univ Nijmegen, Dept Astrophys IMAPP, POB 9010, NL-6500 GL Nijmegen, Netherlands

[10] Inst Astrofis Canarias, Via Lactea S-N, E-38205 San Cristobal la Laguna, Santa Cruz De T, Spain

[11] Univ La Laguna, Dept Astrofis, E-38205 San Cristobal la Laguna, Santa Cruz De T, Spain

[12] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA

[13] Amer Museum Nat Hist, 79th St & Cent Pk West, New York, NY 10024 USA

[14] Univ Lancaster, Dept Phys, Lancaster LA1 4YB, England

[15] Kyoto Sangyo Univ, Koyama Astron Observ, Kita Ku, Kyoto, Kyoto 6038555, Japan

[16] Las Cumbres Observ Global Telescope Network, 6740 Cortona Dr,Suite 102, Goleta, CA 93117 USA

[17] Univ Calif Santa Barbara, Kavli Inst Theoret Phys, Santa Barbara, CA 93106 USA

[18] Russian Acad Sci, Special Astrophys Observ, Nizhnii Arkhyz 369167, Karachai Cherke, Russia

[19] Natl Observ Athens, Inst Astron Astrophys Space Applicat & Remote, Penteli 15236, Greece

[20] Corona Borealis Observ, Ngari, Tibet, Peoples R China

[21] Kazan Fed Univ, Kazan 420008, Russia

[22] Univ Politecn Cataluna, EUETIB, Dept Fis, C-Compte dUrgell 187, E-08036 Barcelona, Spain

[23] Inst dEstudis Espacials Catalunya, C-Gran Capita 2-4,Ed Nexus-201, E-08034 Barcelona, Spain

[24] Xingming Observ, Urumqi, Xinjiang, Peoples R China

[25] NASA, Goddard Space Flight Ctr, Astrophys Sci Div, Greenbelt, MD 20771 USA

[26] Villanova Univ, Dept Astron & Astrophys, 800 Lancaster Ave, Villanova, PA 19085 USA

[27] Moscow MV Lomonosov State Univ, Sternberg Astron Inst, Univ Prospect 13, Moscow 119899, Russia

[28] Clemson Univ, Dept Phys & Astron, Clemson, SC 29634 USA

[29] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

[30] Itagaki Astron Observ, Teppo, Yamagata 9902492, Japan

[31] MiyakiArgenteus Observ, Miyaki, Saga 8401102, Japan

[32] Tokyo Inst Technol, Dept Phys, Meguro Ku, 2-12-1 Ookayama, Tokyo 1528551, Japan

[33] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA

[34] VSOLJ, 7-1 Kitahatsutomi, Kamagaya 2730126, Japan

[35] Charles Univ Prague, Fac Mathemath & Phys, Astron Inst, Holesovickach 2, CR-18000 Prague 8, Czech Republic

[36] Natl Inst Nat Sci, NAOJ, Okayama Astrophys Observ, 3037-5 Honjo, Okayama 7190232, Japan

[37] Nayoro Observ, 157-1 Nisshin, Nayoro, Hokkaido 0960066, Japan

[38] Rikubetsu Space & Earth Sci Museum, Ashoro, Hokkaido 0894301, Japan

[39] Univ Manchester, Jodrell Bank Ctr Astrophys, Alan Turing Bldg, Manchester M13 9PL, Lancs, England

[40] Hokkaido Univ, Fac Sci, Observat & Data Ctr Cosmosci, Kita Ku, Sapporo, Hokkaido 0600810, Japan

[41] Hokkaido Univ, Dept Cosmosci, Kita Ku, Kita 10,Nishi 8, Sapporo, Hokkaido 0600810, Japan

[42] Okayama Univ Sci, Dept Appl Phys, Kita Ku, 1-1 Ridai cho, Okayama, Okayama 7000005, Japan

[43] Univ Washington, Dept Astron, Box 351580, Seattle, WA 98195 USA

[44] Nanjing Putian Telecommun Co Ltd, 1 Putian Rd, Nanjing, Jiangsu 210012, Peoples R China

来源：

ASTROPHYSICAL JOURNAL | 2016年 / 833卷 / 02期

基金：

美国国家航空航天局; 美国国家科学基金会;

关键词：

galaxies: individual (M31); novae cataclysmic variables; stars: individual (M31N 2008-12a); ultraviolet: stars; X-rays: binaries; X-RAY OBSERVATIONS; MULTIWAVELENGTH LIGHT-CURVE; AGAPE MICROLENSING SURVEY; UNIVERSAL DECLINE LAW; UBV COLOR EVOLUTION; SUPER-SOFT PHASE; RS OPHIUCHI 1985; CLASSICAL NOVAE; 2006; OUTBURST; WHITE-DWARFS;

D O I：

10.3847/1538-4357/833/2/149

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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 P-rec = 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 similar to 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 P-rec = 174 +/- 10 days, and we expect the next eruption of M31N 2008-12a. to occur around 2016 mid-September.

引用

页数：38

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