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Magnetic Field Amplification and Saturation by Turbulence in A Relativistic Shock Propagating through An Inhomogeneous Medium

Published online by Cambridge University Press:  22 July 2013

Y. Mizuno ,
M. Pohl ,
J. Niemiec ,
B. Zhang ,
K.-I. Nishikawa  and
P.E. Hardee
Y. Mizuno
Affiliation:
Institute of Astronomy, National Tsing-Hua University, Hsinchu, Taiwan R.O.C.
M. Pohl
Affiliation:
Institute of Physics and Astronomy, Universitat Potsdam, Potsdam-Golm, Germany
J. Niemiec
Affiliation:
Institute of Nuclear Physics PAN, Kraków, Poland
B. Zhang
Affiliation:
Department of Physics and Astronomy, University of Nevada, Las Vegas, NV, USA
K.-I. Nishikawa
Affiliation:
CSPAR, University of Alabama in Huntsville, Huntsville, AL, USA
P.E. Hardee
Affiliation:
Department of Physics and Astronomy, University of Alabama, Tuscaloosa, AL, USA
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Abstract

We perform two-dimensional relativistic magnetohydrodynamic simulations of a mildly relativistic shock propagating through an inhomogeneous medium. Simulation results show that the postshock region becomes turbulent owing to preshock density inhomogeneity, and the magnetic field is strongly amplified due to the stretching and folding of field lines in the turbulent velocity field. The amplified magnetic field evolves into a filamentary structure in two-dimensional simulations. The magnetic energy spectrum is flatter than the Kolmogorov spectrum and indicates that the so-called small-scale dynamo is occurring in the postshock region.

Type
Research Article
Information
European Astronomical Society Publications Series , Volume 61: Gamma-ray Bursts: 15 Years of GRB Afterglows – Progenitors, Environments and Host Galaxies from the Nearby to the Early Universe , 2013 , pp. 173 - 175
Copyright
© EAS, EDP Sciences 2013

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