A 50 s quasi-periodic oscillation in the early X-ray afterglow of GRB 220711B
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| Main Authors: | , , , , , , , , , , , , , , , , , , , , , |
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| Format: | Preprint |
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2025
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| _version_ | 1866918109584031744 |
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| author | Gao, H. Lei, W. -H. Xiao, S. Zhu, Z. -P. Lan, L. Ai, S. -K. Li, A. Xu, N. Wang, T. -C. Zhang, B. Xu, D. Fynbo, J. P. U. Heintz, K. E. Jakobsson, P. Kann, D. A. Fu, S. -Y. Jiang, S. -Q. Liu, X. Xiong, S. -L. Peng, W. -X. Li, X. -B. Xue, W. -C. |
| author_facet | Gao, H. Lei, W. -H. Xiao, S. Zhu, Z. -P. Lan, L. Ai, S. -K. Li, A. Xu, N. Wang, T. -C. Zhang, B. Xu, D. Fynbo, J. P. U. Heintz, K. E. Jakobsson, P. Kann, D. A. Fu, S. -Y. Jiang, S. -Q. Liu, X. Xiong, S. -L. Peng, W. -X. Li, X. -B. Xue, W. -C. |
| contents | It is generally believed that long duration gamma-ray bursts (GRBs) originate from the core collapse of rapidly spinning massive stars and at least some of them are powered by hyper-accreting black holes. However, definite proofs about the progenitor and central engine of these GRBs have not been directly observed in the past. Here we report the existence of a Quasi-Periodic Oscillation (QPO) signature with periodic frequency $\sim$0.02 Hz in the early X-ray afterglow phase of GRB 220711B. Such a low-frequency QPO likely signals the precession of a relativistic jet launched from a GRB hyper-accreting black hole central engine. The energy injection signature from the \textbf{late} X-ray observations (from $5\times 10^2s\sim 1\times10^4s$) is consistent with the precession hypothesis. The prompt $γ$-ray light curve does not show any QPO signature, suggesting that the X-ray flaring emission in the early afterglow phase and prompt emission likely originate from different accretion processess, indicating that the progenitor stars of GRBs have a core-envelope structure with a stratified angular momentum distribution and the late-time accretion disk likely has a misalignment with respect to the rotation axis of the black hole. Such a misalignment is not expected in a canonical collapsar model. As a result, the QPO signature in GRB 220711B may reveal a new formation channel of long GRBs, possibly a stellar-merger-induced core collapse, with the orbital angular momentum of the binary misaligned with the spin axis of the collapsing star. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2508_00278 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | A 50 s quasi-periodic oscillation in the early X-ray afterglow of GRB 220711B Gao, H. Lei, W. -H. Xiao, S. Zhu, Z. -P. Lan, L. Ai, S. -K. Li, A. Xu, N. Wang, T. -C. Zhang, B. Xu, D. Fynbo, J. P. U. Heintz, K. E. Jakobsson, P. Kann, D. A. Fu, S. -Y. Jiang, S. -Q. Liu, X. Xiong, S. -L. Peng, W. -X. Li, X. -B. Xue, W. -C. High Energy Astrophysical Phenomena It is generally believed that long duration gamma-ray bursts (GRBs) originate from the core collapse of rapidly spinning massive stars and at least some of them are powered by hyper-accreting black holes. However, definite proofs about the progenitor and central engine of these GRBs have not been directly observed in the past. Here we report the existence of a Quasi-Periodic Oscillation (QPO) signature with periodic frequency $\sim$0.02 Hz in the early X-ray afterglow phase of GRB 220711B. Such a low-frequency QPO likely signals the precession of a relativistic jet launched from a GRB hyper-accreting black hole central engine. The energy injection signature from the \textbf{late} X-ray observations (from $5\times 10^2s\sim 1\times10^4s$) is consistent with the precession hypothesis. The prompt $γ$-ray light curve does not show any QPO signature, suggesting that the X-ray flaring emission in the early afterglow phase and prompt emission likely originate from different accretion processess, indicating that the progenitor stars of GRBs have a core-envelope structure with a stratified angular momentum distribution and the late-time accretion disk likely has a misalignment with respect to the rotation axis of the black hole. Such a misalignment is not expected in a canonical collapsar model. As a result, the QPO signature in GRB 220711B may reveal a new formation channel of long GRBs, possibly a stellar-merger-induced core collapse, with the orbital angular momentum of the binary misaligned with the spin axis of the collapsing star. |
| title | A 50 s quasi-periodic oscillation in the early X-ray afterglow of GRB 220711B |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2508.00278 |