Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1996
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...461..858s&link_type=abstract
Astrophysical Journal v.461, p.858
Astronomy and Astrophysics
Astronomy
28
Acceleration Of Particles, Gamma Rays: Bursts, Gamma Rays: Theory, Radiation Mechanisms: Nonthermal
Scientific paper
We study the interaction between a magnetized wind that flows away from the γ-ray burster at relativistic speeds and an external medium. In the frame of the outflowing gas, this problem is identical to the problem of collision between a wide relativistic beam of cold plasma and a strong magnetic field. Such a collision is considered numerically. It is assumed that the plasma beam is initially homogeneous and impacts with the Lorentz factor Γ0 ≫ 1 on the magnetic field region, which is called a magnetic barrier. The magnetic field of the barrier is homogeneous and perpendicular to the beam velocity. It is shown that in the process of such a collision, strong electric fields are generated near the front of the magnetic barrier, and electrons are accelerated in these fields. The mean energy of reversed electrons that move away from the barrier is ˜0.05mpc2Γ0 within a factor of 2. The maximum energy of these electrons may be at least ˜½mpc2Γ0. The radiation of accelerated electrons in the vicinity of the barrier front is calculated. In the case of the magnetic field and beam parameters that are relevant to both cosmological γ-ray bursters and an external medium around them, this radiation is in the range of γ-rays. The total energy that can escape from the region of the relativistic beam-magnetic barrier interaction in both γ-rays and high-energy electrons is ˜10%-20% of the beam energy. The fraction of this energy that is radiated in γ-rays immediately at the magnetic barrier may be as high as ˜15% of the beam energy. The results of simulations are used for explanation of observational data on the nonthermal radiation of γ-ray bursters.
Smolsky M. V.
Usov Vladimir V.
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