A Subclass of Gamma-Ray Burst Originating from Compact Binary Merger
Type I gamma-ray bursts (GRBs) are believed to originate from compact binary mergers usually with a duration of main emission less than 2 s. However, recent observations of GRB 211211A and GRB 230307A indicate that some merger-origin GRBs could last much longer. Since they show strikingly similar pr...
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IOP Publishing
2025-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/ad98ec |
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| author | Chen-Wei Wang Wen-Jun Tan Shao-Lin Xiong Shu-Xu Yi Rahim Moradi Bing Li Zhen Zhang Yu Wang Yan-Zhi Meng Bo-Bing Wu Jia-Cong Liu Yue Wang Sheng-Lun Xie Wang-Chen Xue Zheng-Hang Yu Peng Zhang Wen-Long Zhang Yan-Qiu Zhang Chao Zheng |
| author_facet | Chen-Wei Wang Wen-Jun Tan Shao-Lin Xiong Shu-Xu Yi Rahim Moradi Bing Li Zhen Zhang Yu Wang Yan-Zhi Meng Bo-Bing Wu Jia-Cong Liu Yue Wang Sheng-Lun Xie Wang-Chen Xue Zheng-Hang Yu Peng Zhang Wen-Long Zhang Yan-Qiu Zhang Chao Zheng |
| author_sort | Chen-Wei Wang |
| collection | DOAJ |
| description | Type I gamma-ray bursts (GRBs) are believed to originate from compact binary mergers usually with a duration of main emission less than 2 s. However, recent observations of GRB 211211A and GRB 230307A indicate that some merger-origin GRBs could last much longer. Since they show strikingly similar properties (indicating a common mechanism), which are different from the classic “long”-short burst (e.g., GRB 060614), we find they form an interesting subclass of type I GRBs, and we suggest to name them as type IL GRB. We find that the prompt emission of type IL GRB is composed of three episodes: (1) a precursor followed by a short quiescent (or weak emission) period, (2) a long-duration main emission, and (3) an extended emission. With this burst pattern, a good candidate, GRB 170228A, was found in the Fermi/Gamma-ray Burst Monitor archive data. Temporal and spectral analyses indeed show that GRB 170228A falls in the same group with GRB 211211A and GRB 230307A in many diagnostic figures. Thus, this burst pattern could be a good reference for rapidly identifying type IL GRBs and very helpful for conducting low-latency follow-up observation. We estimated the occurrence rate and discussed the physical origins and implications for the three emission episodes of type IL GRBs. Our analysis suggests the premerger precursor model, especially the magnetar super flare model, is more favored for type IL GRBs. More observations in multiwavelength and multimessenger are required to deepen our understanding of this subclass of GRB. |
| format | Article |
| id | doaj-art-796cb947df05489da51ce37396c77e4d |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-796cb947df05489da51ce37396c77e4d2025-01-20T15:18:48ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0197917310.3847/1538-4357/ad98ecA Subclass of Gamma-Ray Burst Originating from Compact Binary MergerChen-Wei Wang0https://orcid.org/0009-0008-8053-2985Wen-Jun Tan1Shao-Lin Xiong2https://orcid.org/0000-0002-4771-7653Shu-Xu Yi3https://orcid.org/0000-0001-7599-0174Rahim Moradi4https://orcid.org/0000-0002-2516-5894Bing Li5https://orcid.org/0000-0002-0238-834XZhen Zhang6https://orcid.org/0000-0003-4673-773XYu Wang7https://orcid.org/0000-0001-7959-3387Yan-Zhi Meng8https://orcid.org/0000-0002-1122-1146Bo-Bing Wu9https://orcid.org/0000-0001-6650-3776Jia-Cong Liu10https://orcid.org/0009-0004-1887-4686Yue Wang11Sheng-Lun Xie12https://orcid.org/0000-0001-9217-7070Wang-Chen Xue13https://orcid.org/0000-0001-8664-5085Zheng-Hang Yu14Peng Zhang15https://orcid.org/0000-0002-8097-3616Wen-Long Zhang16https://orcid.org/0009-0008-6247-0645Yan-Qiu Zhang17https://orcid.org/0000-0001-5348-7033Chao Zheng18https://orcid.org/0009-0001-7226-2355Key Laboratory of Particle Astrophysics, Institute of High Energy Physics , Chinese Academy of Sciences, Beijing 100049, People’s Republic of China ; xiongsl@ihep.ac.cn, sxyi@ihep.ac.cn, rmoradi@ihep.ac.cn; University of Chinese Academy of Sciences , Chinese Academy of Sciences, Beijing 100049, People’s Republic of ChinaKey Laboratory of Particle Astrophysics, Institute of High Energy Physics , Chinese Academy of Sciences, Beijing 100049, People’s Republic of China ; xiongsl@ihep.ac.cn, sxyi@ihep.ac.cn, rmoradi@ihep.ac.cn; University of Chinese Academy of Sciences , Chinese Academy of Sciences, Beijing 100049, People’s Republic of ChinaKey Laboratory of Particle Astrophysics, Institute of High Energy Physics , Chinese Academy of Sciences, Beijing 100049, People’s Republic of China ; xiongsl@ihep.ac.cn, sxyi@ihep.ac.cn, rmoradi@ihep.ac.cnKey Laboratory of Particle Astrophysics, Institute of High Energy Physics , Chinese Academy of Sciences, Beijing 100049, People’s Republic of China ; xiongsl@ihep.ac.cn, sxyi@ihep.ac.cn, rmoradi@ihep.ac.cnKey Laboratory of Particle Astrophysics, Institute of High Energy Physics , Chinese Academy of Sciences, Beijing 100049, People’s Republic of China ; xiongsl@ihep.ac.cn, sxyi@ihep.ac.cn, rmoradi@ihep.ac.cnKey Laboratory of Particle Astrophysics, Institute of High Energy Physics , Chinese Academy of Sciences, Beijing 100049, People’s Republic of China ; xiongsl@ihep.ac.cn, sxyi@ihep.ac.cn, rmoradi@ihep.ac.cnKey Laboratory of Particle Astrophysics, Institute of High Energy Physics , Chinese Academy of Sciences, Beijing 100049, People’s Republic of China ; xiongsl@ihep.ac.cn, sxyi@ihep.ac.cn, rmoradi@ihep.ac.cnICRANet , Piazza della Repubblica 10, I-65122 Pescara, Italy; ICRA, Dipartamento di Fisica, Sapienza Università di Roma , Piazzale Aldo Moro 5, I-00185 Rome, Italy; INAF , Osservatorio Astronomico d’Abruzzo, Via M. Maggini snc, I-64100, Teramo, ItalySchool of Science, Guangxi University of Science and Technology , Liuzhou 545006, People’s Republic of ChinaKey Laboratory of Particle Astrophysics, Institute of High Energy Physics , Chinese Academy of Sciences, Beijing 100049, People’s Republic of China ; xiongsl@ihep.ac.cn, sxyi@ihep.ac.cn, rmoradi@ihep.ac.cnKey Laboratory of Particle Astrophysics, Institute of High Energy Physics , Chinese Academy of Sciences, Beijing 100049, People’s Republic of China ; xiongsl@ihep.ac.cn, sxyi@ihep.ac.cn, rmoradi@ihep.ac.cn; University of Chinese Academy of Sciences , Chinese Academy of Sciences, Beijing 100049, People’s Republic of ChinaKey Laboratory of Particle Astrophysics, Institute of High Energy Physics , Chinese Academy of Sciences, Beijing 100049, People’s Republic of China ; xiongsl@ihep.ac.cn, sxyi@ihep.ac.cn, rmoradi@ihep.ac.cn; University of Chinese Academy of Sciences , Chinese Academy of Sciences, Beijing 100049, People’s Republic of ChinaKey Laboratory of Particle Astrophysics, Institute of High Energy Physics , Chinese Academy of Sciences, Beijing 100049, People’s Republic of China ; xiongsl@ihep.ac.cn, sxyi@ihep.ac.cn, rmoradi@ihep.ac.cn; Institute of Astrophysics, Central China Normal University , Wuhan 430079, People's Republic of ChinaKey Laboratory of Particle Astrophysics, Institute of High Energy Physics , Chinese Academy of Sciences, Beijing 100049, People’s Republic of China ; xiongsl@ihep.ac.cn, sxyi@ihep.ac.cn, rmoradi@ihep.ac.cn; University of Chinese Academy of Sciences , Chinese Academy of Sciences, Beijing 100049, People’s Republic of ChinaKey Laboratory of Particle Astrophysics, Institute of High Energy Physics , Chinese Academy of Sciences, Beijing 100049, People’s Republic of China ; xiongsl@ihep.ac.cn, sxyi@ihep.ac.cn, rmoradi@ihep.ac.cn; University of Chinese Academy of Sciences , Chinese Academy of Sciences, Beijing 100049, People’s Republic of ChinaKey Laboratory of Particle Astrophysics, Institute of High Energy Physics , Chinese Academy of Sciences, Beijing 100049, People’s Republic of China ; xiongsl@ihep.ac.cn, sxyi@ihep.ac.cn, rmoradi@ihep.ac.cn; College of Electronic and Information Engineering, Tongji University , Shanghai 201804, People’s Republic of ChinaKey Laboratory of Particle Astrophysics, Institute of High Energy Physics , Chinese Academy of Sciences, Beijing 100049, People’s Republic of China ; xiongsl@ihep.ac.cn, sxyi@ihep.ac.cn, rmoradi@ihep.ac.cn; School of Physics and Physical Engineering, Qufu Normal University , Qufu, Shandong 273165, People’s Republic of ChinaKey Laboratory of Particle Astrophysics, Institute of High Energy Physics , Chinese Academy of Sciences, Beijing 100049, People’s Republic of China ; xiongsl@ihep.ac.cn, sxyi@ihep.ac.cn, rmoradi@ihep.ac.cn; University of Chinese Academy of Sciences , Chinese Academy of Sciences, Beijing 100049, People’s Republic of ChinaKey Laboratory of Particle Astrophysics, Institute of High Energy Physics , Chinese Academy of Sciences, Beijing 100049, People’s Republic of China ; xiongsl@ihep.ac.cn, sxyi@ihep.ac.cn, rmoradi@ihep.ac.cn; University of Chinese Academy of Sciences , Chinese Academy of Sciences, Beijing 100049, People’s Republic of ChinaType I gamma-ray bursts (GRBs) are believed to originate from compact binary mergers usually with a duration of main emission less than 2 s. However, recent observations of GRB 211211A and GRB 230307A indicate that some merger-origin GRBs could last much longer. Since they show strikingly similar properties (indicating a common mechanism), which are different from the classic “long”-short burst (e.g., GRB 060614), we find they form an interesting subclass of type I GRBs, and we suggest to name them as type IL GRB. We find that the prompt emission of type IL GRB is composed of three episodes: (1) a precursor followed by a short quiescent (or weak emission) period, (2) a long-duration main emission, and (3) an extended emission. With this burst pattern, a good candidate, GRB 170228A, was found in the Fermi/Gamma-ray Burst Monitor archive data. Temporal and spectral analyses indeed show that GRB 170228A falls in the same group with GRB 211211A and GRB 230307A in many diagnostic figures. Thus, this burst pattern could be a good reference for rapidly identifying type IL GRBs and very helpful for conducting low-latency follow-up observation. We estimated the occurrence rate and discussed the physical origins and implications for the three emission episodes of type IL GRBs. Our analysis suggests the premerger precursor model, especially the magnetar super flare model, is more favored for type IL GRBs. More observations in multiwavelength and multimessenger are required to deepen our understanding of this subclass of GRB.https://doi.org/10.3847/1538-4357/ad98ecGamma-ray bursts |
| spellingShingle | Chen-Wei Wang Wen-Jun Tan Shao-Lin Xiong Shu-Xu Yi Rahim Moradi Bing Li Zhen Zhang Yu Wang Yan-Zhi Meng Bo-Bing Wu Jia-Cong Liu Yue Wang Sheng-Lun Xie Wang-Chen Xue Zheng-Hang Yu Peng Zhang Wen-Long Zhang Yan-Qiu Zhang Chao Zheng A Subclass of Gamma-Ray Burst Originating from Compact Binary Merger The Astrophysical Journal Gamma-ray bursts |
| title | A Subclass of Gamma-Ray Burst Originating from Compact Binary Merger |
| title_full | A Subclass of Gamma-Ray Burst Originating from Compact Binary Merger |
| title_fullStr | A Subclass of Gamma-Ray Burst Originating from Compact Binary Merger |
| title_full_unstemmed | A Subclass of Gamma-Ray Burst Originating from Compact Binary Merger |
| title_short | A Subclass of Gamma-Ray Burst Originating from Compact Binary Merger |
| title_sort | subclass of gamma ray burst originating from compact binary merger |
| topic | Gamma-ray bursts |
| url | https://doi.org/10.3847/1538-4357/ad98ec |
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