Generation of Magnetic Fields and Jitter Radiation in GRBs. I. Kinetic Theory

Details Generation of Magnetic Fields and Jitter Radiation in GRBs. I. Kinetic Theory Generation of Magnetic Fields and Jitter Radiation in GRBs. I. Kinetic Theory

2001-02-23

arxiv.org/abs/astro-ph/0102399v1

Astronomy and Astrophysics

Astrophysics

3 pages with 2 eps figures, aipproc.sty. To appear in Proceedings of the 20th Texas Symposium on Relativistic Astrophysics, Au

Scientific paper

10.1063/1.1419628

We present a theory of generation of strong (sub-equipartition) magnetic fields in relativistic collisionless GRB shocks. These fields produced by the kinetic two-stream instability are tangled on very small spatial scales. This has a clear signature in the otherwise synchrotron(-self-Compton) $\gamma$-ray spectrum. Second, we present an analytical theory of jitter radiation, which is emitted when the correlation length of the magnetic field is smaller then the gyration (Larmor) radius of the accelerated electrons. We demonstrate that the spectral power $P(\nu)$ for pure jitter radiation is well-described by a sharply broken power-law: $P(\nu)\propto\nu^1$ for $\nu<\nu_j$ and $P(\nu)\propto\nu^{-(p-1)/2}$ for $\nu>\nu_j$, where $p$ is the electron power-law index and $\nu_j$ is the jitter break, which is independent of the magnetic field strength and depends on the shock energetics and kinematics. Here we mostly focus on the first problem. The radiation theory and comparison with observations will be discussed in the forthcoming publications.

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