Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 478, Issue 1, Pages 926-931Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/sty1159
Keywords
acceleration of particles; shock waves; cosmic rays; pulsars; ISM: supernova remnants
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Funding
- JSPS KAKENHI [JP16K17702, JP16J06773, JP15K05088, JP18H01232]
- MEXT/JSPS Leading Initiative for Excellent Young Researchers
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We propose that cosmic ray PeVatrons are pulsar wind nebulae (PWNe) inside supernova remnants (SNRs). The PWN initially expands into the freely expanding stellar ejecta. Then, the PWN catches up with the shocked region of the SNR, where particles can be slightly accelerated by the back and forth motion between the PWN and the SNR, and some particles diffuse into the PWN. Afterwards the PWN is compressed by the SNR, where the particles in the PWN are accelerated by the adiabatic compression. Using a Monte Carlo simulation, we show that particles accelerated by the SNR to 0.1 PeV can be reaccelerated to 1 PeV until the end of the PWN compression.
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