Shock acceleration with oblique and turbulent magnetic fields
arXiv:2111.04759 · doi:10.3847/1538-4357/ac3824
Abstract
We investigate shock acceleration in a realistic astrophysical environment with density inhomogeneities. The turbulence induced by the interaction of the shock precursor with upstream density fluctuations amplifies both upstream and downstream magnetic fields via the turbulent dynamo. The dynamo-amplified turbulent magnetic fields (a) introduce variations of shock obliquities along the shock face, (b) enable energy gain through a combination of shock drift and diffusive processes, (c) give rise to various spectral indices of accelerated particles, (d) regulate the diffusion of particles both parallel and perpendicular to the magnetic field, and (e) increase the shock acceleration efficiency. Our results demonstrate that upstream density inhomogeneities and dynamo amplification of magnetic fields play an important role in shock acceleration, and thus shock acceleration depends on the condition of the ambient interstellar environment. The implications on understanding radio spectra of supernova remnants are also discussed.
17 pages, 12 figures, accepted for publication in ApJ
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- Cosmic ray streaming in the turbulent interstellar medium
- Turbulent reconnection acceleration
- Quasi-perpendicular shock acceleration and TDE radio flares
- Modeling Hadronic Gamma-ray Emissions from Solar Flares and Prospects for Detecting Non-thermal Signatures from Protostars
- TeV-PeV Gamma-ray and Neutrino Emission in the Galactic Plane