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Simulation of relativistic shocks and associated radiation from turbulent magnetic fields

Published online by Cambridge University Press:  24 February 2011

K.-I. Nishikawa ,
J. Niemiec ,
M. Medvedev ,
B. Zhang ,
P. Hardee ,
Y. Mizuno ,
A. Nordlund ,
J. Frederiksen ,
H. Sol  and
M. Pohl
...Show all authors
K.-I. Nishikawa
Affiliation:
Center for Space Plasma and Aeronomic Research, University of Alabama in Huntsville, NSSTC, 320 Sparkman Drive, Huntsville, AL 35805, USA email: [email protected]
J. Niemiec
Affiliation:
Institute of Nuclear Physics PAN, ul. Radzikowskiego 152, 31-342 Krakow, Poland
M. Medvedev
Affiliation:
Department of Physics and Astronomy, University of Kansas, KS 66045, USA
B. Zhang
Affiliation:
Department of Physics and Astronomy, University of Nevada, Las Vegas, NV 89154, USA
P. Hardee
Affiliation:
Department of Physics and Astronomy, The University of Alabama, Tuscaloosa, AL 35487, USA
Y. Mizuno
Affiliation:
Center for Space Plasma and Aeronomic Research, University of Alabama in Huntsville, NSSTC, 320 Sparkman Drive, Huntsville, AL 35805, USA email: [email protected]
A. Nordlund
Affiliation:
Niels Bohr Institute, Juliane Maries Vej 30, 2100 Kbenhavn, Denmark
J. Frederiksen
Affiliation:
Niels Bohr Institute, Juliane Maries Vej 30, 2100 Kbenhavn, Denmark
H. Sol
Affiliation:
LUTH, Observatore de Paris-Meudon, 5 place Jules Jansen, 92195 Meudon Cedex, France
M. Pohl
Affiliation:
Institut fuer Physik und Astronomie, Universitaet Potsdam, 14476 Potsdam-Golm, Germany
D. H. Hartmann
Affiliation:
Department of Physics and Astronomy, Clemson University, Clemson, SC 29634, USA
G. J. Fishman
Affiliation:
NASA/MSFC, 320 Sparkman Drive, Huntsville, AL 35805, USA
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Abstract

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Recent PIC simulations of relativistic electron-positron (electron-ion) jets injected into a stationary medium show that particle acceleration occurs in the shocked regions. Simulations show that the Weibel instability is responsible for generating and amplifying highly nonuniform, small-scale magnetic fields and for particle acceleration. These magnetic fields contribute to the electron's transverse deflection behind the shock. The “jitter” radiation from deflected electrons in turbulent magnetic fields has different properties from synchrotron radiation calculated in a uniform magnetic field. This jitter radiation may be important for understanding the complex time evolution and/or spectral structure of gamma-ray bursts, relativistic jets in general, and supernova remnants. In order to calculate radiation from first principles and go beyond the standard synchrotron model, we have used PIC simulations. We will present detailed spectra for conditions relevant to various astrophysical sites of collisionless shock formation. In particular we will discuss application to GRBs and SNRs.

Keywords

instabilitiesmagnetic fieldsshock wavesradiation mechanisms: general
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 6 , Symposium S275: Jets at all Scales , September 2010 , pp. 354 - 357
Copyright
Copyright © International Astronomical Union 2011

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