2007/02/28 by Mitsuru Honda
Physics and Astronomy · #Astrophysics and Cosmic Phenomena #Dust and Plasma Wave Phenomena #Magnetic confinement fusion research #astro-ph #physics.plasm-ph
paper · pdf · doi:10.1111/j.1365-2966.2007.11479.x
published as Mon.Not.Roy.Astron.Soc.376:871-880,2007 · 11 pages, 3 figures, matches version published in MNRAS
openalex publication_date 2007/03/06 · arxiv created 2007/04/02 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/30
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 (∼3 × 1024 cm) scales.