GRB 240825A: Early Reverse Shock and Its Physical Implications
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2025
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| author | Wu, Chao Wang, Yun Li, Hua-Li Xin, Li-Ping Xu, Dong Schneider, Benjamin Postigo, Antonio de Ugarte Lamb, Gavin Reguitti, Andrea Saccardi, Andrea Gao, Xing Li, Xing-Ling Wang, Qiu-Li Zhang, Bing Wei, Jian-Yan Zhang, Shuang-Nan Daigne, Frédéric Atteia, Jean-Luc Bernardini, Maria-Grazia Cai, Hong-bo Claret, Arnaud Cordier, Bertrand Deng, Jin-Song Godet, Olivier Götz, Diego Han, Xu-Hui Kang, Zhe Li, Guang-Wei Li, Zhen-Wei Liu, Cheng-Zhi Lu, Xiao-Meng Lv, You Osborne, Julian P Palmerio, Jesse Qiu, Yu-Lei Schanne, Stéphane Turpin, Damien Vergani, Susanna Diana Wang, Jing Xiao, Yu-Jie Xie, Wen-Jin Xu, Yang Yao, Zhu-Heng Zhang, Pin-Pin Zhang, Ruo-Son Zhu, Cheng-Wei Brivio, Riccardo Covino, Stefano D'Avanzo, Paolo Ferro, Matteo Melandri, Andrea Rossi, Andrea Fernández, José Feliciano Agüí Thöne, Christina C. Bai, Chun-Hai Esamdin, Ali Iskandar, Abdusamatjan Yaqup, Shahidin Zhang, Yu Zhong, Tu-Hong Fu, Shao-Yu Jiang, Shuai-Qing Liu, Xing An, Jie Zhu, Zi-Pei Cao, Jia-Xin Liang, En-Wei Lin, Da-Bin Wang, Xiang-Gao Du, Guo-Wang Er, Xin-Zhong Fang, Yuan Liu, Xiao-Wei Adami, Christophe Dennefeld, Michel Floc'h, Emeric Le Fynbo, Johan Peter Uldall Jakobsson, Páll Malesani, Daniele Bjørn Jin, Zhi-Ping Ren, Jia Wang, Hao Wei, Da-Ming Zhou, Hao Campana, Sergio Kobayashi, Shiho De Pasquale, Massimiliano |
| author_facet | Wu, Chao Wang, Yun Li, Hua-Li Xin, Li-Ping Xu, Dong Schneider, Benjamin Postigo, Antonio de Ugarte Lamb, Gavin Reguitti, Andrea Saccardi, Andrea Gao, Xing Li, Xing-Ling Wang, Qiu-Li Zhang, Bing Wei, Jian-Yan Zhang, Shuang-Nan Daigne, Frédéric Atteia, Jean-Luc Bernardini, Maria-Grazia Cai, Hong-bo Claret, Arnaud Cordier, Bertrand Deng, Jin-Song Godet, Olivier Götz, Diego Han, Xu-Hui Kang, Zhe Li, Guang-Wei Li, Zhen-Wei Liu, Cheng-Zhi Lu, Xiao-Meng Lv, You Osborne, Julian P Palmerio, Jesse Qiu, Yu-Lei Schanne, Stéphane Turpin, Damien Vergani, Susanna Diana Wang, Jing Xiao, Yu-Jie Xie, Wen-Jin Xu, Yang Yao, Zhu-Heng Zhang, Pin-Pin Zhang, Ruo-Son Zhu, Cheng-Wei Brivio, Riccardo Covino, Stefano D'Avanzo, Paolo Ferro, Matteo Melandri, Andrea Rossi, Andrea Fernández, José Feliciano Agüí Thöne, Christina C. Bai, Chun-Hai Esamdin, Ali Iskandar, Abdusamatjan Yaqup, Shahidin Zhang, Yu Zhong, Tu-Hong Fu, Shao-Yu Jiang, Shuai-Qing Liu, Xing An, Jie Zhu, Zi-Pei Cao, Jia-Xin Liang, En-Wei Lin, Da-Bin Wang, Xiang-Gao Du, Guo-Wang Er, Xin-Zhong Fang, Yuan Liu, Xiao-Wei Adami, Christophe Dennefeld, Michel Floc'h, Emeric Le Fynbo, Johan Peter Uldall Jakobsson, Páll Malesani, Daniele Bjørn Jin, Zhi-Ping Ren, Jia Wang, Hao Wei, Da-Ming Zhou, Hao Campana, Sergio Kobayashi, Shiho De Pasquale, Massimiliano |
| contents | Early multiwavelength observations offer crucial insights into the nature of the relativistic jets responsible for gamma-ray bursts and their interaction with the surrounding medium.We present data of GRB 240825A from 17 space- and ground-based telescopes/instruments, covering wavelengths from NIR/optical to X-ray and GeV, and spanning from the prompt emission to the afterglow phase triggered by Swift and Fermi. The early afterglow observations were carried out by SVOM/C-GFT, and spectroscopic observations of the afterglow by GTC, VLT, and TNG determined the redshift of the burst ($z = 0.659$) later.A comprehensive analysis of the prompt emission spectrum observed by Swift-BAT and Fermi-GBM/LAT reveals a rare and significant high-energy cutoff at ~76 MeV. Assuming this cutoff is due to $γγ$ absorption allows us to place an upper limit on the initial Lorentz factor, $Γ_0 < 245$. The optical/NIR and GeV afterglow light curves be described by the standard external shock model, with early-time emission dominated by a reverse shock (RS) and a subsequent transition to forward shock (FS) emission. Our afterglow modelling yields a consistent estimate of the initial Lorentz factor ($Γ_{\rm 0} \sim 234$). Furthermore, the RS-to-FS magnetic field ratio ($\mathcal{R}_B \sim 302$) indicates that the reverse shock region is significantly more magnetized than the FS region. An isotropic-equivalent kinetic energy of $E_{\text{k,iso}} = 5.25 \times 10^{54}$ erg is derived, and the corresponding $γ$-ray radiation efficiency is estimated to be $η_γ$ = 3.1%. On the other hand, the standard afterglow model can not reproduce the X-ray light curve of GRB 240825A, calling for improved models to characterize all multiwavelength data. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2507_02806 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | GRB 240825A: Early Reverse Shock and Its Physical Implications Wu, Chao Wang, Yun Li, Hua-Li Xin, Li-Ping Xu, Dong Schneider, Benjamin Postigo, Antonio de Ugarte Lamb, Gavin Reguitti, Andrea Saccardi, Andrea Gao, Xing Li, Xing-Ling Wang, Qiu-Li Zhang, Bing Wei, Jian-Yan Zhang, Shuang-Nan Daigne, Frédéric Atteia, Jean-Luc Bernardini, Maria-Grazia Cai, Hong-bo Claret, Arnaud Cordier, Bertrand Deng, Jin-Song Godet, Olivier Götz, Diego Han, Xu-Hui Kang, Zhe Li, Guang-Wei Li, Zhen-Wei Liu, Cheng-Zhi Lu, Xiao-Meng Lv, You Osborne, Julian P Palmerio, Jesse Qiu, Yu-Lei Schanne, Stéphane Turpin, Damien Vergani, Susanna Diana Wang, Jing Xiao, Yu-Jie Xie, Wen-Jin Xu, Yang Yao, Zhu-Heng Zhang, Pin-Pin Zhang, Ruo-Son Zhu, Cheng-Wei Brivio, Riccardo Covino, Stefano D'Avanzo, Paolo Ferro, Matteo Melandri, Andrea Rossi, Andrea Fernández, José Feliciano Agüí Thöne, Christina C. Bai, Chun-Hai Esamdin, Ali Iskandar, Abdusamatjan Yaqup, Shahidin Zhang, Yu Zhong, Tu-Hong Fu, Shao-Yu Jiang, Shuai-Qing Liu, Xing An, Jie Zhu, Zi-Pei Cao, Jia-Xin Liang, En-Wei Lin, Da-Bin Wang, Xiang-Gao Du, Guo-Wang Er, Xin-Zhong Fang, Yuan Liu, Xiao-Wei Adami, Christophe Dennefeld, Michel Floc'h, Emeric Le Fynbo, Johan Peter Uldall Jakobsson, Páll Malesani, Daniele Bjørn Jin, Zhi-Ping Ren, Jia Wang, Hao Wei, Da-Ming Zhou, Hao Campana, Sergio Kobayashi, Shiho De Pasquale, Massimiliano High Energy Astrophysical Phenomena Early multiwavelength observations offer crucial insights into the nature of the relativistic jets responsible for gamma-ray bursts and their interaction with the surrounding medium.We present data of GRB 240825A from 17 space- and ground-based telescopes/instruments, covering wavelengths from NIR/optical to X-ray and GeV, and spanning from the prompt emission to the afterglow phase triggered by Swift and Fermi. The early afterglow observations were carried out by SVOM/C-GFT, and spectroscopic observations of the afterglow by GTC, VLT, and TNG determined the redshift of the burst ($z = 0.659$) later.A comprehensive analysis of the prompt emission spectrum observed by Swift-BAT and Fermi-GBM/LAT reveals a rare and significant high-energy cutoff at ~76 MeV. Assuming this cutoff is due to $γγ$ absorption allows us to place an upper limit on the initial Lorentz factor, $Γ_0 < 245$. The optical/NIR and GeV afterglow light curves be described by the standard external shock model, with early-time emission dominated by a reverse shock (RS) and a subsequent transition to forward shock (FS) emission. Our afterglow modelling yields a consistent estimate of the initial Lorentz factor ($Γ_{\rm 0} \sim 234$). Furthermore, the RS-to-FS magnetic field ratio ($\mathcal{R}_B \sim 302$) indicates that the reverse shock region is significantly more magnetized than the FS region. An isotropic-equivalent kinetic energy of $E_{\text{k,iso}} = 5.25 \times 10^{54}$ erg is derived, and the corresponding $γ$-ray radiation efficiency is estimated to be $η_γ$ = 3.1%. On the other hand, the standard afterglow model can not reproduce the X-ray light curve of GRB 240825A, calling for improved models to characterize all multiwavelength data. |
| title | GRB 240825A: Early Reverse Shock and Its Physical Implications |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2507.02806 |