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Turbulent amplification of magnetic field and diffusive shock acceleration of cosmic rays
Open accessAbstract
The diffusive shock acceleration of cosmic rays by supernova remnants depends upon the generation of magnetic fluctuations by cosmic rays upstream of the shock. Strongly driven, non-resonant, nearly purely growing modes grow more rapidly than the resonant Alfvén waves usually considered. Non-linear simulation shows that the magnetic field can be amplified from its seed value by orders of magnitude. The consequences for the maximum attainable cosmic ray energy in supernova remnants are explored.
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Citations
Cited by
Acceleration of petaelectronvolt protons in the Galactic Centre
HESS Collaboration (2016) · Nature · doi:10.1038/nature17147 · Cited by 503
The Astrophysics of Ultrahigh-Energy Cosmic Rays
Kotera, K., & Olinto, A. V. (2011) · Annual Review of Astronomy and Astrophysics · doi:10.1146/annurev-astro-081710-102620 · Cited by 470
THE FERMI BUBBLES AS A SCALED-UP VERSION OF SUPERNOVA REMNANTS
Fujita, Y., Ohira, Y., & Yamazaki, R. (2013) · The Astrophysical Journal · doi:10.1088/2041-8205/775/1/l20 · Cited by 47
“CRs are accelerated in the shock neighborhood, where some nonlinear effects generate strong magnetic waves or cause strong amplification of magnetic fields (Lucek & Bell 2000; Bell 2004).”
Background
Metadata
- Authors
- Bell, A. R.
- Venue
- Monthly Notices of the Royal Astronomical Society
- Publisher
- Oxford University Press (OUP)
- Published
- 2004-09
- Volume
- 353
- Issue
- 2
- Pages
- 550-558
- ISSN
- 0035-8711 (ISSN-L)
- 1365-2966
- OpenAlex
- W2032882333
- Cited by
- 1,148
- References
- 0
- FWCI
- 12.66
- Type
- journal article
- Language
- en
- Open access
- bronze
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- Bell, A. R. (2004). Turbulent amplification of magnetic field and diffusive shock acceleration of cosmic rays. Monthly Notices of the Royal Astronomical Society. https://doi.org/10.1111/j.1365-2966.2004.08097.x
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