A novel explosive process is required for the γ-ray burst GRB 060614

被引:350
作者
Gal-Yam, A. [1 ]
Fox, D. B.
Price, P. A.
Ofek, E. O.
Davis, M. R.
Leonard, D. C.
Soderberg, A. M.
Schmidt, B. P.
Lewis, K. M.
Peterson, B. A.
Kulkarni, S. R.
Berger, E.
Cenko, S. B.
Sari, R.
Sharon, K.
Frail, D.
Moon, D. -S.
Brown, P. J.
Cucchiara, A.
Harrison, F.
Piran, T.
Persson, S. E.
McCarthy, P. J.
Penprase, B. E.
Chevalier, R. A.
MacFadyen, A. I.
机构
[1] CALTECH, Div Phys Math & Astron, Pasadena, CA 91125 USA
[2] Penn State Univ, Dept Astron & Astrophys, Davey Lab 525, University Pk, PA 16802 USA
[3] Univ Hawaii, Inst Astron, Honolulu, HI 96822 USA
[4] San Diego State Univ, Dept Astron, San Diego, CA 92182 USA
[5] Australian Natl Univ, Mt Stromlo Observ, Res Sch Astron & Astrophys, Weston, ACT 2611, Australia
[6] Carnegie Inst Washington Observ, Pasadena, CA 91101 USA
[7] Princeton Univ Observ, Princeton, NJ 08544 USA
[8] Tel Aviv Univ, Dept Astrophys, IL-69978 Tel Aviv, Israel
[9] Natl Radio Astron Observ, Socorro, NM 87801 USA
[10] Hebrew Univ Jerusalem, Racah Inst Phys, IL-91904 Jerusalem, Israel
[11] Pomona Coll, Dept Phys & Astron, Claremont, CA 91711 USA
[12] Univ Virginia, Dept Astron, Charlottesville, VA 22904 USA
[13] Inst Adv Study, Princeton, NJ 08540 USA
[14] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA
基金
美国国家航空航天局; 美国国家科学基金会;
关键词
D O I
10.1038/nature05373
中图分类号
O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];
学科分类号
07 ; 0710 ; 09 ;
摘要
Over the past decade, our physical understanding of gamma-ray bursts (GRBs) has progressed rapidly, thanks to the discovery and observation of their long-lived afterglow emission. Long-duration (greater than or similar to 2 s) GRBs are associated with the explosive deaths of massive stars ('collapsars', ref. 1), which produce accompanying supernovae(2-5); the short- duration (less than or similar to 2 s) GRBs have a different origin, which has been argued to be the merger of two compact objects(6-9). Here we report optical observations of GRB 060614 (duration 100 s, ref. 10) that rule out the presence of an associated supernova. This would seem to require a new explosive process: either a massive collapsar that powers a GRB without any associated supernova, or a new type of 'engine', as long-lived as the collapsar but without a massive star. We also show that the properties of the host galaxy (redshift z = 0.125) distinguish it from other long-duration GRB hosts and suggest that an entirely new type of GRB progenitor may be required.
引用
收藏
页码:1053 / 1055
页数:3
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