Resolution dependence of magnetosheath waves in global hybrid-Vlasov simulations

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Dubart , M , Ganse , U , Osmane , A , Johlander , A , Battarbee , M , Grandin , M , Pfau-Kempf , Y , Turc , L & Palmroth , M 2020 , ' Resolution dependence of magnetosheath waves in global hybrid-Vlasov simulations ' , Annales Geophysicae , vol. 38 , no. 6 , pp. 1283-1298 . https://doi.org/10.5194/angeo-38-1283-2020

Title: Resolution dependence of magnetosheath waves in global hybrid-Vlasov simulations
Author: Dubart, Maxime; Ganse, Urs; Osmane, Adnane; Johlander, Andreas; Battarbee, Markus; Grandin, Maxime; Pfau-Kempf, Yann; Turc, Lucile; Palmroth, Minna
Contributor: University of Helsinki, Space Physics Research Group
University of Helsinki, Department of Physics
University of Helsinki, Department of Physics
University of Helsinki, Space Physics Research Group
University of Helsinki, Space Physics Research Group
University of Helsinki, Particle Physics and Astrophysics
University of Helsinki, Particle Physics and Astrophysics
University of Helsinki, Space Physics Research Group
University of Helsinki, Department of Physics
Date: 2020-12-21
Language: eng
Number of pages: 16
Belongs to series: Annales Geophysicae
ISSN: 0992-7689
URI: http://hdl.handle.net/10138/324518
Abstract: Kinetically driven plasma waves are fundamental for a description of the thermodynamical properties of the Earth's magnetosheath. The most commonly observed ion-scale instabilities are generated by temperature anisotropy of the ions, such as the mirror and proton cyclotron instabilities. We investigate here the spatial resolution dependence of the mirror and proton cyclotron instabilities in a global hybrid-Vlasov simulation using the Vlasiator model; we do this in order to find optimal resolutions and help future global hybrid-Vlasov simulations to save resources when investigating those instabilities in the magnetosheath. We compare the proton velocity distribution functions, power spectra and growth rates of the instabilities in a set of simulations with three different spatial resolutions but otherwise identical setup. We find that the proton cyclotron instability is absent at the lowest resolution and that only the mirror instability remains, which leads to an increased temperature anisotropy in the simulation. We conclude that the proton cyclotron instability, its saturation and the reduction of the anisotropy to marginal levels are resolved at the highest spatial resolution. A further increase in resolution does not lead to a better description of the instability to an extent that would justify this increase at the cost of numerical resources in future simulations. We also find that spatial resolutions between 1.32 and 2.64 times the inertial length in the solar wind present acceptable limits for the resolution within which the velocity distribution functions resulting from the proton cyclotron instability are still bi-Maxwellian and reach marginal stability levels. Our results allow us to determine a range of spatial resolutions suitable for the modelling of the proton cyclotron and mirror instabilities and should be taken into consideration regarding the optimal grid spacing for the modelling of these two instabilities, within available computational resources.
Subject: ELECTRON-TEMPERATURE ANISOTROPY
MIRROR MODE STRUCTURES
MAGNETIC-FIELD
ION DISTRIBUTIONS
EARTHS FORESHOCK
BOW SHOCK
ET-AL.
INSTABILITY
PLASMA
FLUCTUATIONS
115 Astronomy, Space science
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