| GEOPHYSICS, ASTRONOMY, AND ASTROPHYSICS |
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Characteristics of Double Gamma-Ray Bursts |
| LIU Tong1,2,3**, SUN Mou-Yuan1,4, HOU Shu-Jin1,5, LI Ang1,3, ZHANG Fu-Wen6, GU Wei-Min1, LU Ju-Fu1 |
1Department of Astronomy and Institute of Theoretical Physics and Astrophysics, Xiamen University, Xiamen 361005
2Key Laboratory for the Structure and Evolution of Celestial Objects, Chinese Academy of Sciences, Kunming 650011
3State Key Laboratory of Theoretical Physics, Institute of Theoretical Physics, Chinese Academy of Sciences, Beijing 100190
4Department of Astronomy and Astrophysics and Institute for Gravitation and the Cosmos, Pennsylvania State University, University Park, PA 16802, USA
5College of Physics and Electronic Engineering, Nanyang Normal University, Nanyang 473061
6College of Science, Guilin University of Technology, Guilin 541004
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| Cite this article: |
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LIU Tong, SUN Mou-Yuan, HOU Shu-Jin et al 2014 Chin. Phys. Lett. 31 119801 |
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Abstract Double gamma-ray bursts (DGRBs) have two well-separated sub-bursts in the main prompt emission and the typical time interval between them is in the hundreds of seconds. Among DGRBs, gamma-ray bursts (DGRBs) 110801A and 120716A are the ones with known redshifts. However, unlike GRB 110801A, we show that the two sub-bursts of GRB 120716A is severally similar to the short- and long-duration GRBs, thus it is difficult to explain the origin of GRB 120716A by the popular models on the central engine of GRBs. We suggest that some mechanisms of x-ray flares in GRBs, i.e., a post-merger millisecond pulsars or the jet precession in a black hole hyperaccretion system may produce the DGRB.
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Published: 28 November 2014
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| PACS: |
98.70.Rz
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(γ-ray sources; γ-ray bursts)
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