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| Main Authors: | , |
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| Format: | Preprint |
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2024
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| Online Access: | https://arxiv.org/abs/2406.07244 |
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| _version_ | 1866910655435505664 |
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| author | Kazuki, Kamiido Yutaka, Ohira |
| author_facet | Kazuki, Kamiido Yutaka, Ohira |
| contents | In this work, we investigate collisionless shocks propagating in a relativistically hot unmagnetized electron-positron plasmas. We estimate the dissipation fraction at shocks in the relativistically hot plasma, showing that it is sufficiently large to explain the observation of gamma-ray bursts even when the shock is not highly relativistic. It is shown by two-dimensional particle in cell simulations that magnetic fields are generated around the shock front by the Weibel instability, as in the cold upstream plasma. However, in contrast to the cold upstream plasma, no particles are accelerated at the shock in the simulation time of $t = 3600 ω_p^{-1}$. The decay of the magnetic field in the downstream region is slower for slower shock velocities in the hot plasma cases. Applying the slow decay of the downstream magnetic field, we propose a model that generate magnetic fields in large downstream region, which is required from the standard model of the gamma-ray burst afterglow. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2406_07244 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Collisionless shock in a relativistically hot unmagnetized electron-positron plasma Kazuki, Kamiido Yutaka, Ohira High Energy Astrophysical Phenomena In this work, we investigate collisionless shocks propagating in a relativistically hot unmagnetized electron-positron plasmas. We estimate the dissipation fraction at shocks in the relativistically hot plasma, showing that it is sufficiently large to explain the observation of gamma-ray bursts even when the shock is not highly relativistic. It is shown by two-dimensional particle in cell simulations that magnetic fields are generated around the shock front by the Weibel instability, as in the cold upstream plasma. However, in contrast to the cold upstream plasma, no particles are accelerated at the shock in the simulation time of $t = 3600 ω_p^{-1}$. The decay of the magnetic field in the downstream region is slower for slower shock velocities in the hot plasma cases. Applying the slow decay of the downstream magnetic field, we propose a model that generate magnetic fields in large downstream region, which is required from the standard model of the gamma-ray burst afterglow. |
| title | Collisionless shock in a relativistically hot unmagnetized electron-positron plasma |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2406.07244 |