Understanding Streaming Instabilities in the Limit of High Cosmic Ray Current Density
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arXiv
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| Main Authors: | , , , |
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| Format: | Preprint |
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2024
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| _version_ | 1866929705236561920 |
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| author | Lichko, Emily Caprioli, Damiano Schroer, Benedikt Gupta, Siddhartha |
| author_facet | Lichko, Emily Caprioli, Damiano Schroer, Benedikt Gupta, Siddhartha |
| contents | A critical component of particle acceleration in astrophysical shocks is the non-resonant (Bell) instability, where the streaming of cosmic rays (CRs) leads to the amplification of magnetic fields necessary to scatter particles. In this work we use kinetic particle-in-cells simulations to investigate the high-CR current regime, where the typical assumptions underlying the Bell instability break down. Despite being more strongly driven, significantly less magnetic field amplification is observed compared to low-current cases, an effect due to the anisotropic heating that occurs in this regime. We also find that electron-scale modes, despite being fastest growing, mostly lead to moderate electron heating and do not affect the late evolution or saturation of the instability. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2411_05704 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Understanding Streaming Instabilities in the Limit of High Cosmic Ray Current Density Lichko, Emily Caprioli, Damiano Schroer, Benedikt Gupta, Siddhartha High Energy Astrophysical Phenomena Plasma Physics A critical component of particle acceleration in astrophysical shocks is the non-resonant (Bell) instability, where the streaming of cosmic rays (CRs) leads to the amplification of magnetic fields necessary to scatter particles. In this work we use kinetic particle-in-cells simulations to investigate the high-CR current regime, where the typical assumptions underlying the Bell instability break down. Despite being more strongly driven, significantly less magnetic field amplification is observed compared to low-current cases, an effect due to the anisotropic heating that occurs in this regime. We also find that electron-scale modes, despite being fastest growing, mostly lead to moderate electron heating and do not affect the late evolution or saturation of the instability. |
| title | Understanding Streaming Instabilities in the Limit of High Cosmic Ray Current Density |
| topic | High Energy Astrophysical Phenomena Plasma Physics |
| url | https://arxiv.org/abs/2411.05704 |