Magnetic field generation in relativistic shocks

Free access article

Issue		A&A Volume 428, Number 2, December III 2004


Page(s)		365 - 371
Section		Astrophysical processes
DOI		http://dx.doi.org/10.1051/0004-6361:20041882

A&A 428, 365-371 (2004)
DOI: 10.1051/0004-6361:20041882

An early end of the exponential Weibel instability in electron-proton plasmas

J. Wiersma and A. Achterberg

Sterrenkundig Instituut, Universiteit Utrecht, PO Box 80000, 3508 TA Utrecht, The Netherlands
e-mail: wiersma@astro.uu.nl

(Received 21 April 2004 / Accepted 26 August 2004)

Abstract
We discuss magnetic field generation by the proton Weibel instability in relativistic shocks, a situation that applies to the external shocks in the fireball model for Gamma-ray Bursts, and possibly also to internal shocks. Our analytical estimates show that the linear phase of the instability ends well before it has converted a significant fraction of the energy in the proton beam into magnetic energy: the conversion efficiency is much smaller (of order $m_{\rm e}/m_{\rm p}$ ) in electron-proton plasmas than in pair plasmas. We find this estimate by modelling the plasma in the shock transition zone with a waterbag momentum distribution for the protons and with a background of hot electrons.

For ultra-relativistic shocks we find that the wavelength of the most efficient mode for magnetic field generation equals the electron skin depth, that the relevant nonlinear stabilization mechanism is magnetic trapping, and that the presence of the hot electrons limits the typical magnetic field strength generated by this mode so that it does not depend on the energy content of the protons. We conclude that other processes than the linear Weibel instability must convert the free energy of the protons into magnetic fields.

Key words: plasmas -- magnetic fields -- instabilities -- shock waves -- gamma rays: bursts

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