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Magnetised Wave Collapse in Solar System Plasmas

Published online by Cambridge University Press:  25 April 2016

Andrew Melatos  and
Peter Robinson
Andrew Melatos
Affiliation:
Department of Theoretical Physics and Research Centre for Theoretical Astrophysics, School of Physics, University of Sydney, NSW 2006
Peter Robinson
Affiliation:
Department of Theoretical Physics and Research Centre for Theoretical Astrophysics, School of Physics, University of Sydney, NSW 2006
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Abstract

Clumpy, intense wave packets observed in situ in the Jovian and terrestrial electron foreshocks, and in the Earth’s auroral acceleration zone, point to the existence of non-linear plasma turbulence in these regions. In non-linear turbulence, wave packets collapse to short scales and high fields, stopping only when coherent wave-particle interactions efficiently dissipate the energy in the waves. The purpose of this paper is to examine the shortest scales and highest fields achieved during collapse in a strongly magnetised plasma, and identify parts of the solar system where the magnetised aspects of wave collapse are important.

Type
Solar and Solar System
Information
Publications of the Astronomical Society of Australia , Volume 10 , Issue 4 , 1993 , pp. 283 - 286
Copyright
Copyright © Astronomical Society of Australia 1993

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