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A kinetic model of plasma turbulence

Part of: Present Achievements in SpacePlasmas Focus on Space Plasmas

Published online by Cambridge University Press:  10 October 2014

S. Servidio ,
F. Valentini ,
D. Perrone ,
A. Greco ,
F. Califano ,
W. H. Matthaeus  and
P. Veltri
S. Servidio*
Affiliation:
Dipartimento di Fisica, Universitá della Calabria, Cosenza, 87036, Italy
F. Valentini
Affiliation:
Dipartimento di Fisica, Universitá della Calabria, Cosenza, 87036, Italy
D. Perrone
Affiliation:
LESIA, Observatoire de Paris, 92190 Meudon, France
A. Greco
Affiliation:
Dipartimento di Fisica, Universitá della Calabria, Cosenza, 87036, Italy
F. Califano
Affiliation:
Dipartimento di Fisica and CNISM, Universitá di Pisa, Pisa, 56127, Italy
W. H. Matthaeus
Affiliation:
Bartol Research Institute and Department of Physics and Astronomy, University of Delaware, Newark, DE 19716, USA
P. Veltri
Affiliation:
Dipartimento di Fisica, Universitá della Calabria, Cosenza, 87036, Italy
*
†Email address for correspondence: [email protected]
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Abstract

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A Hybrid Vlasov–Maxwell (HVM) model is presented and recent results about the link between kinetic effects and turbulence are reviewed. Using five-dimensional (2D in space and 3D in the velocity space) simulations of plasma turbulence, it is found that kinetic effects (or non-fluid effects) manifest through the deformation of the proton velocity distribution function (DF), with patterns of non-Maxwellian features being concentrated near regions of strong magnetic gradients. The direction of the proper temperature anisotropy, calculated in the main reference frame of the distribution itself, has a finite probability of being along or across the ambient magnetic field, in general agreement with the classical definition of anisotropy T⊥/T∥ (where subscripts refer to the magnetic field direction). Adopting the latter conventional definition, by varying the global plasma beta (β) and fluctuation level, simulations explore distinct regions of the space given by T⊥/T∥ and β∥, recovering solar wind observations. Moreover, as in the solar wind, HVM simulations suggest that proton anisotropy is not only associated with magnetic intermittent events, but also with gradient-type structures in the flow and in the density. The role of alpha particles is reviewed using multi-ion kinetic simulations, revealing a similarity between proton and helium non-Maxwellian effects. The techniques presented here are applied to 1D spacecraft-like analysis, establishing a link between non-fluid phenomena and solar wind magnetic discontinuities. Finally, the dimensionality of turbulence is investigated, for the first time, via 6D HVM simulations (3D in both spaces). These preliminary results provide support for several previously reported studies based on 2.5D simulations, confirming several basic conclusions. This connection between kinetic features and turbulence open a new path on the study of processes such as heating, particle acceleration, and temperature-anisotropy, commonly observed in space plasmas.

Type
Research Article
Information
Journal of Plasma Physics , Volume 81 , Issue 1 , January 2015 , 325810107
Copyright
Copyright © Cambridge University Press 2014 

References

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