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Kinetic Alfvén wave generation by velocity shear in collisionless plasmas

Part of: Focus on Plasma Astrophysics The Many Facets of the Vlasov Equation

Published online by Cambridge University Press:  23 April 2020

Teresa Maiorano ,
Adriana Settino Open the ORCID record for Adriana Settino [Opens in a new window] ,
Francesco Malara Open the ORCID record for Francesco Malara [Opens in a new window] ,
Oreste Pezzi Open the ORCID record for Oreste Pezzi [Opens in a new window] ,
Francesco Pucci Open the ORCID record for Francesco Pucci [Opens in a new window]  and
Francesco Valentini Open the ORCID record for Francesco Valentini [Opens in a new window]
Teresa Maiorano
Affiliation:
Dipartimento di Fisica, Università della Calabria, 87036 Rende (CS), Italy
Adriana Settino
Affiliation:
Dipartimento di Fisica, Università della Calabria, 87036 Rende (CS), Italy
Francesco Malara*
Affiliation:
Dipartimento di Fisica, Università della Calabria, 87036 Rende (CS), Italy
Oreste Pezzi
Affiliation:
Gran Sasso Science Institute, Viale F. Crispi 7, I-67100 L. Aquila, Italy INFN/Laboratori Nazionali del Gran Sasso, Via G. Acitelli 22, I-67100 Assergi (AQ), Italy
Francesco Pucci
Affiliation:
Centre for Mathematical Plasma Astrophysics, Department of Mathematics, KU Leuven, Celestijnenlaan 200B, 3001Leuven, Belgium
Francesco Valentini
Affiliation:
Dipartimento di Fisica, Università della Calabria, 87036 Rende (CS), Italy
*
†Email address for correspondence: [email protected]
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Abstract

The evolution of a linearly polarized, long-wavelength Alfvén wave propagating in a collisionless magnetized plasma with a sheared parallel-directed velocity flow is here studied by means of two-dimensional hybrid Vlasov–Maxwell (HVM) simulations. The unperturbed sheared flow has been represented by an exact solution of the HVM set of equations of (Malara et al., Phys. Rev. E, vol. 97, 2018, 053212), thus avoiding spurious oscillations that would arise from the non-stationary initial state and inevitably affect the dynamics of the system. We have considered the evolution of both a small and a moderate amplitude Alfvén wave, in order to separate linear wave–shear flow couplings from kinetic effects, the latter being more relevant for larger wave amplitudes. The phase mixing generated by the shear flow modifies the initial perturbation, leading to the formation of small-scale transverse fluctuations at scales comparable with the proton inertial length/Larmor radius. By analysing both the polarization and group velocity of perturbations in the shear regions, we identify them as kinetic Alfvén waves (KAWs). In the moderate amplitude run, kinetic effects distort the proton distribution function in the shear region. This leads to the formation of a proton beam, at the Alfvén speed and parallel to the magnetic field. Such a feature, due to the parallel electric field associated with KAWs, positively compares with solar wind observations of suprathermal ion populations, suggesting that it may be related to the presence of ion-scale KAW-like fluctuations.

Keywords

plasma simulationplasma wavesspace plasma physics
Type
Research Article
Information
Journal of Plasma Physics , Volume 86 , Issue 2 , April 2020 , 825860202
Copyright
© Cambridge University Press 2020

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