An upper limit to the energy of gamma-ray bursts indicates that GRBs/SNe are powered by magnetars

被引：99
作者：
Mazzali, P. A. [1 ,2 ,3 ]
McFadyen, A. I. [4 ]
Woosley, S. E. [5 ]
Pian, E. [6 ]
Tanaka, M. [7 ]
机构：
[1] Liverpool John Moores Univ, Astrophys Res Inst, Liverpool L3 5RF, Merseyside, England
[2] INAF Osservatorio Astron, I-35122 Padua, Italy
[3] Max Planck Inst Astrophys, D-85748 Garching, Germany
[4] NYU, Dept Phys, Ctr Cosmol & Particle Phys, New York, NY 10003 USA
[5] Univ Calif Santa Cruz, Dept Astron & Astrophys, Santa Cruz, CA 95064 USA
[6] INAF IASF, I-40129 Bologna, Italy
[7] Natl Astron Observ Japan, Mitaka, Tokyo 1818588, Japan
来源：
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2014年 / 443卷 / 01期
关键词：
gamma-ray burst: general; stars: magnetars; supernovae: general; OPTICAL AFTERGLOW; NEUTRON-STAR; SN; 1998BW; E-P; E-I-E-ISO CORRELATION; HYPERNOVA EXPLOSIONS; RELATIVISTIC JETS; SUPERNOVA; 2003DH; CENTRAL ENGINE; LIGHT CURVES; GRB; 130427A;
D O I：
10.1093/mnras/stu1124
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
The kinetic energy of supernovae (SNe) accompanied by gamma-ray bursts (GRBs) tends to cluster near 10(52) erg, with 2 x 10(52) erg an upper limit to which no compelling exceptions are found (assuming a certain degree of asphericity), and it is always significantly larger than the intrinsic energy of the GRB themselves (corrected for jet collimation). This energy is strikingly similar to the maximum rotational energy of a neutron star rotating with period 1 ms. It is therefore proposed that all GRBs associated with luminous SNe are produced by magnetars. GRBs that result from black hole formation (collapsars) may not produce luminous SNe. X-ray flashes, which are associated with less energetic SNe, are produced by neutron stars with weaker magnetic field or lower spin.
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页码：67 / 71
页数：5
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