Issue |
A&A
Volume 676, August 2023
|
|
---|---|---|
Article Number | L3 | |
Number of page(s) | 6 | |
Section | Letters to the Editor | |
DOI | https://doi.org/10.1051/0004-6361/202245401 | |
Published online | 28 July 2023 |
Letter to the Editor
Cosmic-ray electrons and the magnetic field of the North Polar Spur
1
Department of Astronomy, School of Physics and Technology, Wuhan University, Wuhan 430072, PR China
e-mail: gbmou@whu.edu.cn
2
Department of Physics and Institute of Theoretical Physics, The Chinese University of Hong Kong, Shatin, Hong Kong, SAR, China
3
School of Computer Science, Wuhan University, Wuhan 430072, PR China
4
Institute of Astronomy, The University of Tokyo, Mitaka, Tokyo 181-0015, Japan
Received:
8
November
2022
Accepted:
15
July
2023
Aims. The recent confirmation of the bipolarity of the eROSITA bubbles suggests that the well-known North Polar Spur (NPS)/Loop I probably is a 10 kpc sized relic in the Galactic halo and not a small local structure near the Sun. By virtue of multiwavelength observations of the NPS, unprecedentedly precise parameter constraints on the cosmic-ray electrons (CRes) and magnetic field in the post-shock halo medium can be provided.
Methods. The parameters of the CRes and the magnetic field can be derived independently by modeling the gamma-ray and the radio data of the NPS via inverse Compton scattering and synchrotron emission, respectively.
Results. Our main results are (1) that the energy density of the CRe is (3–6)×10−14 erg cm−3, and the spectral index below the cooling break energy of about 5 GeV is p ≃ 2.0 ± 0.1; (2) that the magnetic field strength is 3 μG; and (3) that the shock acceleration efficiency of the CRe is (1–2)%. Given the Mach number of 1.5, the high acceleration efficiency and flat spectrum of the CRe suggest that preexisting relativistic electrons may be reaccelerated in the NPS. Alternatively, these CRes could be accelerated by an evolving shock in the early epoch when the Mach number is high, and efficiently diffuse throughout the post-shock halo gas. In addition, the cooling break energy suggests that the cooling timescale is 107 yr, which agrees with the age of the eROSITA bubbles.
Key words: acceleration of particles / radiation mechanisms: non-thermal / evolution / Galaxy: halo / shock waves / ISM: structure
© The Authors 2023
Open Access article, published by EDP Sciences, under the terms of the Creative Commons Attribution License (https://creativecommons.org/licenses/by/4.0), which permits unrestricted use, distribution, and reproduction in any medium, provided the original work is properly cited.
This article is published in open access under the Subscribe to Open model. Subscribe to A&A to support open access publication.
Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.
Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.
Initial download of the metrics may take a while.