Propagation and escape of astrophysical cyclotron-maser radiation

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]. The resultant radiation sig...

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Bibliographic Details
Published in2013 Abstracts IEEE International Conference on Plasma Science (ICOPS) p. 1
Main Authors Speirs, D. C., Gillespie, K. M., Ronald, K., McConville, S. L., Robertson, C. W., Phelps, A. D. R., Cross, A. W., Bingham, R., Kellett, B. J., Cairns, R. A., Vorgul, I.
Format Conference Proceeding
LanguageEnglish
Published IEEE 01.06.2013
Subjects
Couplings
Cyclotrons
Educational institutions
Electric potential
Magnetic fields
Physics
Plasmas
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Summary: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]. 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 [1][2], there are numerous potential hindrances to the propagation and escape of the radiation from the source region, including second harmonic cyclotron absorption [3] and coupling onto the dispersion branch connecting with vacuum propagation.
ISSN:0730-9244
2576-7208
DOI:10.1109/PLASMA.2013.6635229