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Rapid cosmic-ray acceleration at perpendicular shocks in supernova remnants

MPG-Autoren
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Takamoto,  Makoto
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;
Department of Earth and Planetary Science, The University of Tokyo, 7-3-1 Hongo, Bunkyo-ku, Tokyo 113-0033, Japan;

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Kirk,  John G.
Division Prof. Dr. Werner Hofmann, MPI for Nuclear Physics, Max Planck Society;

Volltexte (frei zugänglich)

1506.04354.pdf
(Preprint), 268KB

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Zitation

Takamoto, M., & Kirk, J. G. (2015). Rapid cosmic-ray acceleration at perpendicular shocks in supernova remnants. The Astronomical Journal, 89(1): 29. doi:10.1088/0004-637X/809/1/29.


Zitierlink: http://hdl.handle.net/11858/00-001M-0000-0028-9F08-A
Zusammenfassung
Perpendicular shocks are shown to be rapid particle accelerators that perform optimally when the ratio us of the shock speed to the particle speed roughly equals the ratio 1/η of the scattering rate to the gyro frequency. We use analytical methods and Monte-Carlo simulations to solve the kinetic equation that governs the anisotropy generated at these shocks, and find, for ηus ≈ 1, that the spectral index softens by unity and the acceleration time increases by a factor of two compared to the standard result of the diffusive shock acceleration theory. These results provide a theoretical basis for the 30 year old conjecture that a supernova exploding into the wind of a Wolf–Rayet star may accelerate protons to an energy exceeding 1015 eV.