Hydrogen-rich supernovae beyond the neutrino-driven core-collapse paradigm

被引：51

作者：

Terreran, G. ^{[1
,2
,3
]}

Pumo, M. L. ^{[2
,4
,5
]}

Chen, T. -W. ^{[6
]}

Moriya, T. J. ^{[7
]}

Taddia, F. ^{[8
]}

Dessart, L. ^{[9
]}

Zampieri, L. ^{[2
]}

Smartt, S. J. ^{[1
]}

Benetti, S. ^{[2
]}

Inserra, C. ^{[1
]}

Cappellaro, E. ^{[2
]}

Nicholl, M. ^{[10
]}

Fraser, M. ^{[11
]}

Wyrzykowski, L. ^{[12
]}

Udalski, A. ^{[12
]}

Howell, D. A. ^{[13
,14
]}

McCully, C. ^{[13
,14
]}

Valenti, S. ^{[15
]}

Dimitriadis, G. ^{[16
]}

Maguire, K. ^{[1
]}

Sullivan, M. ^{[16
]}

Smith, K. W. ^{[1
]}

Yaron, O. ^{[17
]}

Young, D. R. ^{[1
]}

Anderson, J. P. ^{[18
]}

Della Valle, M. ^{[19
,20
]}

Elias-Rosa, N. ^{[2
]}

Gal-Yam, A. ^{[17
]}

Jerkstrand, A. ^{[21
]}

Kankare, E. ^{[1
]}

Pastorello, A. ^{[2
]}

Sollerman, J. ^{[8
]}

Turatto, M. ^{[2
]}

Kostrzewa-Rutkowska, Z. ^{[12
,22
,23
]}

Kozlowski, S. ^{[12
]}

Mroz, P. ^{[12
]}

Pawlak, M. ^{[12
]}

Pietrukowicz, P. ^{[12
,24
]}

Poleski, R. ^{[12
]}

Skowron, D. ^{[12
]}

Skowron, J. ^{[12
]}

Soszynski, I. ^{[12
]}

Szymanski, M. K. ^{[12
]}

Ulaczyk, K. ^{[12
,25
]}

机构：

[1] Queens Univ Belfast, Sch Math & Phys, Astrophys Res Ctr, Belfast BT7 1NN, Antrim, North Ireland

[2] INAF Osservatorio Astron Padova, Vicolo Osservatorio 5, I-35122 Padua, Italy

[3] Univ Padua, Dipartimento Fis & Astron G Galilei, Vicolo Osservatorio 3, I-35122 Padua, Italy

[4] Univ Catania, Dipartimento Fis & Astron, Via Santa Sofia 64, I-95123 Catania, Italy

[5] INFN Lab Nazl Sud, Via Santa Sofia 62, I-95123 Catania, Italy

[6] Max Planck Inst Extraterr Phys, Giessenbachstr E1, D-85748 Garching, Germany

[7] Natl Inst Nat Sci, Natl Astron Observ Japan, Div Theoret Astron, 2-21-1 Osawa, Mitaka, Tokyo 1818588, Japan

[8] Stockholm Univ, AlbaNova, Dept Astron, Oskar Klein Ctr, S-10691 Stockholm, Sweden

[9] Univ Chile, Dept Astron, Unidad Mixta Int Francochilena Astron CNRS UMI 33, Camino El Observ 1515, Santiago, Chile

[10] Harvard Smithsonian Ctr Astrophys, 60 Garden St, Cambridge, MA 02138 USA

[11] Univ Coll Dublin, OBrien Ctr Sci North, Sch Phys, Dublin 4, Ireland

[12] Univ Warsaw Observ, Al Ujazdowskie 4, PL-00478 Warsaw, Poland

[13] Las Cumbres Observ, 6740 Cortona Dr Suite 102, Goleta, CA 93117 USA

[14] Univ Calif Santa Barbara, Dept Phys, Broida Hall,Mail Code 9530, Santa Barbara, CA 93106 USA

[15] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA

[16] Univ Southampton, Dept Phys & Astron, Southampton SO17 1BJ, Hants, England

[17] Weizmann Inst Sci, Dept Particle Phys & Astrophys, IL-76100 Rehovot, Israel

[18] European Southern Observ, Alonso Cordova 3107,Casilla 19, Santiago, Chile

[19] INAF Osservatorio Astron Capodimonte, I-80131 Naples, Italy

[20] Int Ctr Relativist Astrophys, Piazza Repubbl,10, I-65122 Pescara, Italy

[21] Max Planck Inst Astrophys, Karl Schwarzschild Str 1, D-85741 Garching, Germany

[22] SRON Netherlands Inst Space Res, Sorbonnelaan 2, NL-3584 CA Utrecht, Netherlands

[23] Radboud Univ Nijmegen, Inst Math Astrophys & Particle Phys, Dept Astrophys, POB 9010, NL-6500 GL Nijmegen, Netherlands

[24] Ohio State Univ, Dept Astron, 140 West 18th Ave, Columbus, OH 43210 USA

[25] Univ Warwick, Dept Phys, Gibbet Hill Rd, Coventry CV4 7AL, W Midlands, England

来源：

NATURE ASTRONOMY | 2017年 / 1卷 / 10期

基金：

美国国家科学基金会; 欧洲研究理事会; 日本学术振兴会; 英国科学技术设施理事会; 爱尔兰科学基金会; 以色列科学基金会;

关键词：

II PLATEAU SUPERNOVAE; LIGHT CURVES; GALAXIES; STELLAR; METALLICITY; PROGENITORS; ULTRAVIOLET; EXPLOSIONS; PHOTOMETRY; 2009KF;

D O I：

10.1038/s41550-017-0228-8

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Type II supernovae are the final stage of massive stars (above 8 M-circle dot) which retain part of their hydrogen-rich envelope at the moment of explosion. They typically eject up to 15 M-circle dot of material, with peak magnitudes of -17.5 mag and energies in the order of 10(51) erg, which can be explained by neutrino-driven explosions and neutron star formation. Here, we present our study of OGLE-2014-SN-073, one of the brightest type II supernovae ever discovered, with an unusually broad lightcurve combined with high ejecta velocities. From our hydrodynamical modelling, we infer a remarkable ejecta mass of 60(-16)(+42) M-circle dot and a relatively high explosion energy of 12.4(-5.9)(+13.0) x 10(51) erg. We show that this object belongs, along with a very small number of other hydrogen-rich supernovae, to an energy regime that is not explained by standard core-collapse neutrino-driven explosions. We compare the quantities inferred by the hydrodynamical modelling with the expectations of various exploding scenarios and attempt to explain the high energy and luminosity released. We find some qualitative similarities with pair-instability supernovae, although the prompt injection of energy by a magnetar seems to be a viable alternative explanation for such an extreme event.

引用

页码：713 / 720

页数：8

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