Suppression of resistive hose instability in a relativistic electron-positron flow

Details Suppression of resistive hose instability in a relativistic electron-positron flow Suppression of resistive hose instability in a relativistic electron-positron flow

2007-02-14

arxiv.org/abs/astro-ph/0702398v2

Mon.Not.Roy.Astron.Soc.376:871-880,2007

Astronomy and Astrophysics

Astrophysics

11 pages, 3 figures, matches version published in MNRAS

Scientific paper

10.1111/j.1365-2966.2007.11479.x

This paper presents the effects of electron-positron pair production on the linear growth of the resistive hose instability of a filamentary beam that could lead to snake-like distortion. For both the rectangular radial density profile and the diffuse profile reflecting the Bennett-type equilibrium for a self-collimating flow, the modified eigenvalue equations are derived from a Vlasov-Maxwell equation. While for the simple rectangular profile, current perturbation is localized at the sharp radial edge, for the realistic Bennett profile with an obscure edge, it is non-locally distributed over the entire beam, removing catastrophic wave-particle resonance. The pair production effects likely decrease the betatron frequency, and expand the beam radius to increase the resistive decay time of the perturbed current; these also lead to a reduction of the growth rate. It is shown that, for the Bennett profile case, the characteristic growth distance for a preferential mode can exceed the observational length-scale of astrophysical jets. This might provide the key to the problem of the stabilized transport of the astrophysical jets including extragalactic jets up to Mpc ($\sim 3\times 10^{24}$ cm) scales.

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