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dc.contributor.authorZhang, Ming
dc.date.accessioned2016-10-21T14:07:03Z
dc.date.available2016-10-21T14:07:03Z
dc.date.issued2015-10-20
dc.identifier.citationZhang, M. (2015). STOCHASTIC ACCELERATION of GALACTIC COSMIC RAYS by COMPRESSIBLE PLASMA FLUCTUATIONS in SUPERNOVA SHELLS. Astrophysical Journal, 812(2) doi:10.1088/0004-637X/812/2/148en_US
dc.identifier.urihttp://hdl.handle.net/11141/1087
dc.description.abstractA theory of 2-stage acceleration of Galactic cosmic rays in supernova remnants is proposed. The first stage is accomplished by the supernova shock front, where a power-law spectrum is established up to a certain cutoff energy. It is followed by stochastic acceleration with compressible waves/turbulence in the downstream medium. With a broad ∝k^(-2) spectrum for the compressible plasma fluctuations, the rate of stochastic acceleration is constant over a wide range of particle momentum. In this case, the stochastic acceleration process extends the power-law spectrum cutoff energy of Galactic cosmic rays to the knee without changing the spectral slope. This situation happens as long as the rate of stochastic acceleration is faster than 1/5 of the adiabatic cooling rate. A steeper spectrum of compressible plasma fluctuations that concentrate their power in long wavelengths will accelerate cosmic rays to the knee with a small bump before its cutoff in the comic-ray energy spectrum. This theory does not require a strong amplification of the magnetic field in the upstream interstellar medium in order to accelerate cosmic rays to the knee energy.en_US
dc.language.isoen_USen_US
dc.rightsThis published article is made available in accordance with the publisher’s policy. It may be subject to U.S. copyright law.en_US
dc.rights.urihttps://aas.org/publications/aas-copyright-policyen_US
dc.titleSTOCHASTIC ACCELERATION of GALACTIC COSMIC RAYS by COMPRESSIBLE PLASMA FLUCTUATIONS in SUPERNOVA SHELLSen_US
dc.typeArticleen_US
dc.identifier.doi10.1088/0004-637X/812/2/148


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