Nishikawa 2008 Relativistic simulatioin of GRB prompt and early afterglow

主要内容:
including jitter and synchrotron

精彩摘抄:


文章信息:

· Find Similar Abstracts (with default settings below)

· arXiv e-print (arXiv:0809.5067)

· References in the Article

·

· Translate This Page

Title:		New Relativistic Particle-In-Cell Simulation Studies of Prompt and Early Afterglows from GRBs
Authors:		Nishikawa, K. -I.; Niemiec, J.; Sol, H.; Medvedev, M.; Zhang, B.; Nordlund, A.; Fredriksen, J.; Hardee, P.; Mizuno, Y.; Hartmann, D. H.; Fishman, G. J.
Publication:		eprint arXiv:0809.5067
Publication Date:		09/2008
Origin:		ARXIV
Keywords:		Astrophysics
Comment:		: 4 pages, 1 figure and 1 table, submitted for the Proceedings of The 4th Heidelberg International Symposium on High Energy Gamma-Ray Astronomy, July 7-11, 2008, in Heidelberg, Germany
Bibliographic Code:		2008arXiv0809.5067N

Abstract

Nonthermal radiation observed from astrophysical systems containing relativistic jets and shocks, e.g., gamma-ray bursts (GRBs), active galactic nuclei (AGNs), and microquasars commonly exhibit power-law emission spectra. Recent PIC simulations of relativistic electron-ion (or electron-positron) jets injected into a stationary medium show that particle acceleration occurs within the downstream jet. In collisionless, relativistic shocks, particle (electron, positron, and ion) acceleration is due to plasma waves and their associated instabilities (e.g., the Weibel (filamentation) instability) created in the shock region. The simulations show that the Weibel instability is responsible for generating and amplifying highly non-uniform, small-scale magnetic fields. These fields contribute to the electron's transverse deflection behind the jet head. The resulting "jitter" radiation from deflected electrons has different properties compared to synchrotron radiation, which assumes a uniform magnetic field. Jitter radiation may be important for understanding the complex time evolution and/or spectra in gamma-ray bursts, relativistic jets in general, and supernova remnants.

---

Bibtex entry for this abstract Preferred format for this abstract (see Preferences)