GRB 211024B: an ultra-long GRB powered by magnetar
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| Main Authors: | , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866916449373650944 |
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| author | Fu, Shao-Yu Xu, Dong Lei, Wei-Hua Postigo, Antonio de Ugarte Malesani, Daniele B. Kann, David Alexander Jakobsson, Páll Fynbo, Johan P. U. Maiorano, Elisabetta Rossi, Andrea Paris, Diego Liu, Xing Jiang, Shuai-Qing Lu, Tian-Hua An, Jie Zhu, Zi-Pei Gao, Xing Wei, Jian-Yan |
| author_facet | Fu, Shao-Yu Xu, Dong Lei, Wei-Hua Postigo, Antonio de Ugarte Malesani, Daniele B. Kann, David Alexander Jakobsson, Páll Fynbo, Johan P. U. Maiorano, Elisabetta Rossi, Andrea Paris, Diego Liu, Xing Jiang, Shuai-Qing Lu, Tian-Hua An, Jie Zhu, Zi-Pei Gao, Xing Wei, Jian-Yan |
| contents | Ultra-long gamma-ray bursts (ULGRBs) are characterized by exceptionally long-duration central engine activities, with characteristic timescales exceeding 1000 seconds. We present ground-based optical afterglow observations of the ultra-long gamma-ray burst GRB 211024B, detected by \textit{Swift}. Its X-ray light curve exhibits a characteristic ``internal plateau" with a shallow decay phase lasting approximately $\sim 15$ ks, followed by a steep decline ($α_{\rm drop}\sim-7.5$). Moreover, the early optical emission predicted by the late r-band optical afterglow is significantly higher than the observed value, indicating an external shock with energy injection. To explain these observations, we propose a magnetar central engine model. The magnetar collapse into a black hole due to spin-down or hyperaccretion, leading to the observed steep break in the X-ray light curve. The afterglow model fitting reveals that the afterglow injection luminosity varies with different assumptions of the circumburst medium density, implying different potential energy sources. For the interstellar medium (ISM) case with a fixed injection end time, the energy may originate from the magnetar's dipole radiation. However, in other scenarios, relativistic jets produced by the magnetar/black hole system could be the primary energy source. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2410_15162 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | GRB 211024B: an ultra-long GRB powered by magnetar Fu, Shao-Yu Xu, Dong Lei, Wei-Hua Postigo, Antonio de Ugarte Malesani, Daniele B. Kann, David Alexander Jakobsson, Páll Fynbo, Johan P. U. Maiorano, Elisabetta Rossi, Andrea Paris, Diego Liu, Xing Jiang, Shuai-Qing Lu, Tian-Hua An, Jie Zhu, Zi-Pei Gao, Xing Wei, Jian-Yan High Energy Astrophysical Phenomena Ultra-long gamma-ray bursts (ULGRBs) are characterized by exceptionally long-duration central engine activities, with characteristic timescales exceeding 1000 seconds. We present ground-based optical afterglow observations of the ultra-long gamma-ray burst GRB 211024B, detected by \textit{Swift}. Its X-ray light curve exhibits a characteristic ``internal plateau" with a shallow decay phase lasting approximately $\sim 15$ ks, followed by a steep decline ($α_{\rm drop}\sim-7.5$). Moreover, the early optical emission predicted by the late r-band optical afterglow is significantly higher than the observed value, indicating an external shock with energy injection. To explain these observations, we propose a magnetar central engine model. The magnetar collapse into a black hole due to spin-down or hyperaccretion, leading to the observed steep break in the X-ray light curve. The afterglow model fitting reveals that the afterglow injection luminosity varies with different assumptions of the circumburst medium density, implying different potential energy sources. For the interstellar medium (ISM) case with a fixed injection end time, the energy may originate from the magnetar's dipole radiation. However, in other scenarios, relativistic jets produced by the magnetar/black hole system could be the primary energy source. |
| title | GRB 211024B: an ultra-long GRB powered by magnetar |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2410.15162 |