Polarized synchrotron data and the structure of the Galactic magnetic field
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arXiv
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| Natura: | Preprint |
| Pubblicazione: |
2024
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| _version_ | 1866909550553071616 |
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| author | Becker, C. T. Kachelriess, M. |
| author_facet | Becker, C. T. Kachelriess, M. |
| contents | The polarized synchrotron data of the northern C-BASS survey show a surprisingly low linear polarization fraction, $Π\simeq 3\%$, while the magnetic field polarization features coherent structures over rather large angular scales. The low polarization degree points to a strong dominance of the turbulent magnetic field -- in agreement with the observation that the total synchrotron intensity is much larger than expected from the regular component in current models for the Galactic magnetic field (GMF). In contrast, studies of cosmic ray propagation employing these GMF models suggest that cosmic rays propagate anisotropically, what in turn requires weak turbulent fields. As a solution to this contradicting requirements, we suggest that the GMF consists of three components with different levels of turbulence: a disk dominated by the turbulent field, a halo dominated by the regular field, plus an extended turbulent halo field. |
| format | Preprint |
| id |
arxiv_https___arxiv_org_abs_2408_02554 |
| institution | arXiv |
| publishDate | 2024 |
| record_format | arxiv |
| spellingShingle | Polarized synchrotron data and the structure of the Galactic magnetic field Becker, C. T. Kachelriess, M. Astrophysics of Galaxies The polarized synchrotron data of the northern C-BASS survey show a surprisingly low linear polarization fraction, $Π\simeq 3\%$, while the magnetic field polarization features coherent structures over rather large angular scales. The low polarization degree points to a strong dominance of the turbulent magnetic field -- in agreement with the observation that the total synchrotron intensity is much larger than expected from the regular component in current models for the Galactic magnetic field (GMF). In contrast, studies of cosmic ray propagation employing these GMF models suggest that cosmic rays propagate anisotropically, what in turn requires weak turbulent fields. As a solution to this contradicting requirements, we suggest that the GMF consists of three components with different levels of turbulence: a disk dominated by the turbulent field, a halo dominated by the regular field, plus an extended turbulent halo field. |
| title | Polarized synchrotron data and the structure of the Galactic magnetic field |
| topic | Astrophysics of Galaxies |
| url | https://arxiv.org/abs/2408.02554 |