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| Auteurs principaux: | , , , , , , , , , , , |
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| Format: | Preprint |
| Publié: |
2025
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| Accès en ligne: | https://arxiv.org/abs/2509.05628 |
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| _version_ | 1866911141119131648 |
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| author | Maccary, R. Guidorzi, C. Maistrello, M. Kobayashi, S. Bulla, M. Moradi, R. Yi, S. -X. Wang, C. W. Zhang, W. L. Tan, W. -J. Xiong, S. -L Zhang, S. -N. |
| author_facet | Maccary, R. Guidorzi, C. Maistrello, M. Kobayashi, S. Bulla, M. Moradi, R. Yi, S. -X. Wang, C. W. Zhang, W. L. Tan, W. -J. Xiong, S. -L Zhang, S. -N. |
| contents | Short gamma-ray bursts (SGRBs), occasionally followed by a long and spectrally soft extended emission, are associated with compact object mergers (COMs). Yet, a few recent long GRBs (LGRBs) show compelling evidence for a COM origin, in contrast with the massive-star core-collapse origin of most LGRBs. While possible COM indicators were found, such as the minimum variability timescale (MVT), a detailed and unique characterisation of their gamma-ray prompt emission that may help identify and explain their deceptively long profile is yet to be found. Here we report the discovery of a set of distinctive properties that rule the temporal and spectral evolution of GRB 230307A, a LGRB with evidence for a COM origin. Specifically, the sequence of pulses that make up its profile is characterised by an exponential evolution of (i) flux intensities, (ii) waiting times between adjacent pulses, (iii) pulse durations, and (iv) spectral peak energy. Analogous patterns are observed in the prompt emission of other long COM candidates. The observed evolution of gamma-ray pulses would imply that a relativistic jet is colliding with more slowly expanding material. This contrasts with the standard internal shock model for typical LGRBs, in which dissipation occurs at random locations within the jet itself. We tentatively propose a few simple toy models that may explain these properties and are able to reproduce the overall time profile. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2509_05628 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | A set of distinctive properties ruling the prompt emission of GRB 230307A and other long γ-ray bursts from compact object mergers Maccary, R. Guidorzi, C. Maistrello, M. Kobayashi, S. Bulla, M. Moradi, R. Yi, S. -X. Wang, C. W. Zhang, W. L. Tan, W. -J. Xiong, S. -L Zhang, S. -N. High Energy Astrophysical Phenomena Short gamma-ray bursts (SGRBs), occasionally followed by a long and spectrally soft extended emission, are associated with compact object mergers (COMs). Yet, a few recent long GRBs (LGRBs) show compelling evidence for a COM origin, in contrast with the massive-star core-collapse origin of most LGRBs. While possible COM indicators were found, such as the minimum variability timescale (MVT), a detailed and unique characterisation of their gamma-ray prompt emission that may help identify and explain their deceptively long profile is yet to be found. Here we report the discovery of a set of distinctive properties that rule the temporal and spectral evolution of GRB 230307A, a LGRB with evidence for a COM origin. Specifically, the sequence of pulses that make up its profile is characterised by an exponential evolution of (i) flux intensities, (ii) waiting times between adjacent pulses, (iii) pulse durations, and (iv) spectral peak energy. Analogous patterns are observed in the prompt emission of other long COM candidates. The observed evolution of gamma-ray pulses would imply that a relativistic jet is colliding with more slowly expanding material. This contrasts with the standard internal shock model for typical LGRBs, in which dissipation occurs at random locations within the jet itself. We tentatively propose a few simple toy models that may explain these properties and are able to reproduce the overall time profile. |
| title | A set of distinctive properties ruling the prompt emission of GRB 230307A and other long γ-ray bursts from compact object mergers |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2509.05628 |