Propagation and escape of astrophysical cyclotron-maser radiation

David C Speirs , Karen Gillespie, Kevin Ronald, Sandra L McConville , Sandra L McConville , Alan D R Phelps , Alan D R Phelps , Adrian W Cross , Robert Bingham, Barry J Kellett, Robert A Cairns, Irena Vorgul

Research output: Chapter in Book/Report/Conference proceedingConference contribution

Abstract

A multitude of astrophysical plasma environments exist where a combination of particle acceleration, convergent magnetic fields and a sufficiently large ratio of electron cyclotron frequency to plasma frequency are present to support electron cyclotron-maser emission [1-6]. The resultant radiation signatures typically comprise of well-defined spectral components (around the relativistic electron cyclotron frequency) with near 100% left or right handed circular polarization when viewed out-with the source region. Although the generation mechanism has been well documented [7-25], there are numerous potential hindrances to the propagation and escape of the radiation from the source region, including issues of geometry/mode conversion [26] and coupling onto the dispersion branch connecting with vacuum propagation [12]. In the current context we consider the results of numerical Particle-in-cell (PiC) simulations conducted at the University of Strathclyde to study the spatial growth rate and emission topology of the cyclotron-maser emission process. The results have significant bearing on the radiation propagation characteristics and highly debated question of propagation/escape, with particular relevance to the planetary/stellar auroral magnetospheric case.
Original languageEnglish
Title of host publication19th IEEE Pulsed Power Conference (PPC)
Number of pages8
Publication statusPublished - 2013
Externally publishedYes

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