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| Main Authors: | , , |
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| Format: | Preprint |
| Published: |
2024
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| Subjects: | |
| Online Access: | https://arxiv.org/abs/2404.03903 |
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| _version_ | 1866929303736811520 |
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| author | Inoue, Tsuyoshi Marcowith, Alexandre Giacinti, Gwenael |
| author_facet | Inoue, Tsuyoshi Marcowith, Alexandre Giacinti, Gwenael |
| contents | Supernova blast wave shock is a very important site of cosmic-ray acceleration. However, the detailed physical process of acceleration, in particular, non-linear interplay between cosmic-ray streaming and magnetic field amplification has not been studied under a realistic environment. In this paper, using a unique and novel numerical method, we study cosmic-ray acceleration at supernova blast wave shock propagating in the interstellar medium with well-resolved magnetic field amplification by non-resonant hybrid instability (or Bell instability). We find that the magnetic field is mildly amplified under typical ISM conditions that leads to maximum cosmic-ray energy ~30 TeV for supernova remnants with age ~1000 years consistent with gamma-ray observations. The strength of the amplified magnetic field does not reach so-called saturation level, because cosmic-ray electric current towards the shock upstream has finite spatial extent, by which Bell instability cannot experience many e-folding times. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2404_03903 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Bell Instability-Mediated Diffusive Shock Acceleration at Supernova Blast Wave Shock Propagating in the ISM Inoue, Tsuyoshi Marcowith, Alexandre Giacinti, Gwenael High Energy Astrophysical Phenomena Supernova blast wave shock is a very important site of cosmic-ray acceleration. However, the detailed physical process of acceleration, in particular, non-linear interplay between cosmic-ray streaming and magnetic field amplification has not been studied under a realistic environment. In this paper, using a unique and novel numerical method, we study cosmic-ray acceleration at supernova blast wave shock propagating in the interstellar medium with well-resolved magnetic field amplification by non-resonant hybrid instability (or Bell instability). We find that the magnetic field is mildly amplified under typical ISM conditions that leads to maximum cosmic-ray energy ~30 TeV for supernova remnants with age ~1000 years consistent with gamma-ray observations. The strength of the amplified magnetic field does not reach so-called saturation level, because cosmic-ray electric current towards the shock upstream has finite spatial extent, by which Bell instability cannot experience many e-folding times. |
| title | Bell Instability-Mediated Diffusive Shock Acceleration at Supernova Blast Wave Shock Propagating in the ISM |
| topic | High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2404.03903 |