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

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dc.creatorHonda, Mitsuru
dc.date2007-02-14
dc.date2007-04-02
dc.date.accessioned2026-07-07T10:21:47Z
dc.date.available2026-07-07T10:21:47Z
dc.descriptionThis 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.
dc.description11 pages, 3 figures, matches version published in MNRAS
dc.identifierhttps://arxiv.org/abs/astro-ph/0702398
dc.identifierhttp://arxiv.org/abs/astro-ph/0702398
dc.identifierMon.Not.Roy.Astron.Soc.376:871-880,2007
dc.identifierdoi:10.1111/j.1365-2966.2007.11479.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/175292
dc.subjectAstrophysics
dc.subjectPlasma Physics
dc.titleSuppression of resistive hose instability in a relativistic electron-positron flow
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