Magnetic Field Generation and Subsequent Field Dissipation with Plasma Heating in Relativistic Streaming Pair Plasmas

Details Magnetic Field Generation and Subsequent Field Dissipation with Plasma Heating in Relativistic Streaming Pair Plasmas Magnetic Field Generation and Subsequent Field Dissipation with Plasma Heating in Relativistic Streaming Pair Plasmas

Aug 2000

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2000jpsj...69.2503s&link_type=abstract

Journal of the Physical Society of Japan, Volume 69, Issue 8, pp. 2503 (2000).

Astronomy and Astrophysics

Astrophysics

6

Scientific paper

Relativistic plasma streaming in background plasmas becomes unstableagainst the Weibel-type electromagnetic instability, which is one ofeffective mechanisms of magnetic field generation in cosmic plasmas. It isshown by using 3-D fully relativistic particle-in-cell (PIC) simulation codethat magnetic fields perpendicular to the stream in an electron-positron(pair) plasma are generated in the early stage of the instability withsmall-scale sizes of the electron skin-depth. In the subsequent nonlinearstage there occurs magnetic reconnection which causes to make large-scalestructure of magnetic fields in pair plasmas. The magnetic field dissipationthrough the magnetic reconnection leads to heating of the background plasma.These sequential physical processes are important for understanding ofmagnetic field generation in the relativistic shock of gamma-ray burst (GRB)sources in astrophysical plasmas.

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