Open AccessSuppression of resistive hose instability in a relativistic electron–positron flow
Author(s) -
Honda Mitsuru
Publication year - 2007
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2007.11479.x
Subject(s) - physics , instability , betatron , radius , resistive touchscreen , electron , computational physics , gyroradius , beam (structure) , mechanics , quantum electrodynamics , atomic physics , nuclear physics , optics , computer security , electrical engineering , engineering , computer science
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 × 10 24 cm) scales.