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Radiation from accelerated particles in shocks

Published online by Cambridge University Press:  05 September 2012

K.-I. Nishikawa
Affiliation:
Center for Space Plasma and Aeronomic Research, University of Alabama in Huntsville, 320 Sparkman Drive, Huntsville, AL 35805, USA email: ken-ichi.nishikawa-1@nasa.gov
B. Zhang
Affiliation:
Department of Physics and Astronomy, University of Nevada, Las Vegas, NV 89154, USA
E. J. Choi
Affiliation:
Korea Advanced Institute of Science and Technology, Daejeon 305-701, South Korea
K. W. Min
Affiliation:
Korea Advanced Institute of Science and Technology, Daejeon 305-701, South Korea
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
P. Hardee
Affiliation:
Department of Physics and Astronomy, The University of Alabama, Tuscaloosa, AL 35487, USA
Y. Mizuno
Affiliation:
Institute of Astronomy, National Tsing-Hua University, No. 101, Sec. 2, Kuang-Fu Road., Hsinchu, Taiwan 30013, R.O.C.
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 properties different 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 present synthetic spectra to compare with the spectra obtained from Fermi observations.

Type
Poster Papers
Copyright
Copyright © International Astronomical Union 2012

References

Abdo, A. A., et al. 2009, Science, 323, 1688Google Scholar
Medvedev, M. V. 2006, ApJ, 637, 869CrossRefGoogle Scholar
Nishikawa, K.-I., et al. 2009b, ApJ, 689, L10CrossRefGoogle Scholar
Nishikawa, K.-I., et al. 2011, AdvSR, 47, 1434Google Scholar