A new 3‐D spherical hybrid model for solar wind interaction studies

Dyadechkin, Sergey; Kallio, Esa; Järvinen, R.

doi:10.1002/jgra.50497

Cited by 11 publications

(15 citation statements)

References 31 publications

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“…Kallio et al [] used a hierarchical Cartesian grid, but their lowest resolution close to the obstacle is still 180 km, which forces them to introduce a fluid ion background to mimic the ionosphere. More recently, the same group has developed a 3‐D global spherical hybrid model for Venus [ Dyadechkin et al , ], with a minimum radial resolution of 200 km. The model gives a promising result but is not yet applied to the Mars‐solar wind interaction.…”

Section: Simulation Resultsmentioning

confidence: 99%

Mars‐solar wind interaction: LatHyS, an improved parallel 3‐D multispecies hybrid model

et al. 2016

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In order to better represent Mars‐solar wind interaction, we present an unprecedented model achieving spatial resolution down to 50 km, a so far unexplored resolution for global kinetic models of the Martian ionized environment. Such resolution approaches the ionospheric plasma scale height. In practice, the model is derived from a first version described in Modolo et al. (2005). An important effort of parallelization has been conducted and is presented here. A better description of the ionosphere was also implemented including ionospheric chemistry, electrical conductivities, and a drag force modeling the ion‐neutral collisions in the ionosphere. This new version of the code, named LatHyS (Latmos Hybrid Simulation), is here used to characterize the impact of various spatial resolutions on simulation results. In addition, and following a global model challenge effort, we present the results of simulation run for three cases which allow addressing the effect of the suprathermal corona and of the solar EUV activity on the magnetospheric plasma boundaries and on the global escape. Simulation results showed that global patterns are relatively similar for the different spatial resolution runs, but finest grid runs provide a better representation of the ionosphere and display more details of the planetary plasma dynamic. Simulation results suggest that a significant fraction of escaping O+ ions is originated from below 1200 km altitude.

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Section: Simulation Resultsmentioning

confidence: 99%

Mars‐solar wind interaction: LatHyS, an improved parallel 3‐D multispecies hybrid model

et al. 2016

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“…Previously, stretched spherical meshes were employed to conduct 2D (Lin, 2003) and 3D (Lin & Wang, 2005) hybrid simulations of the Earth's magnetosphere. A spherical mesh was also used in the hybrid simulations of solar wind interactions with planets like Venus by Dyadechkin et al (2013). We note, however, that results from hybrid simulations, carried out on spherical and Cartesian meshes, may be somewhat different, as demonstrated by Dyadechkin et al (2013).…”

Section: Space Adaptivitymentioning

confidence: 99%

3D Space‐Time Adaptive Hybrid Simulations of Magnetosheath High‐Speed Jets

Omelchenko

Chen

2021

JGR Space Physics

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Many transient physical processes operate simultaneously and couple nonlinearly in the near-Earth environment across turbulent spatio-temporal scales, producing strong impacts on the cusp, magnetopause and ionosphere that are difficult to fully understand and predict without kinetic simulations. In particular, under quasi-radial interplanetary magnetic field (IMF) conditions the turbulent magnetosheath flow generates large-amplitude, spatially localized dynamic pressure enhancements, known as magnetosheath jets or high-speed jets (Plaschke et al., 2018). These structures, commonly observed by satellites downstream of quasi-parallel bow shocks, carry significant amounts of momentum, energy and magnetic flux. Therefore, their generation mechanism, characteristic lifetimes, physical and geometric properties, and possible impact on the magnetosphere present strong interest to the space physics community.Based on observations in the past two decades, a great amount of statistical knowledge, as well as possible theoretical explanations relating the occurrence of jets to solar wind and foreshock conditions, have been accumulated (Plaschke et al., 2018(Plaschke et al., , 2020. In particular, a theory by Hietala et al. (2012Hietala et al. ( , 2009 suggests that plasma ripples, which inherently develop in the bow shock under quasi-radial IMF and high Mach solar wind conditions, may be responsible for producing local high-speed flows in the magnetosheath by deflecting the incoming solar wind plasma flow in the anti-sunward direction due to the local curvature of a shock front so that the speed of the deflected flow remains close to the upstream solar wind value.

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“…The model runs at equilibrium in under t f = 300 s and has a typical timestep ∆t ∼ 10 −3 s, small enough to converge towards a quasi-stationary state that satisfies the Courant-Friedrichs-Lewy condition needed for a stable numerical integration of the QNH equations (Birdsall 1991). For a more technical description, the reader is referred to Kallio & Jarvinen (2012) and, for the spherical version of the QNH model, to Dyadechkin et al (2013).…”

Section: Quasi-neutral Hybrid Architecturementioning

confidence: 99%

Hybrid modelling of cometary plasma environments

Wedlund

Alho

Gronoff

et al. 2017

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Context. The ESA/Rosetta mission made it possible to monitor the plasma environment of a comet, from near aphelion to perihelion conditions. To understand the complex dynamics and plasma structures found at the comet, a modelling effort must be carried out in parallel. Aims. Firstly, we present a 3D hybrid model of the cometary plasma environment including photoionisation, solar wind charge exchange, and electron ionisation reactions; this model is used in stationary and dynamic conditions (mimicking the solar wind variations), and is thus especially adapted to a weakly outgassing comet such as 67P/Churyumov-Gerasimenko, the target of the ESA/Rosetta mission. Secondly, we use the model to study the respective effects of ionisation processes on the formation of the dayside macroscopic magnetic and density boundaries upstream of comet 67P in perihelion conditions at 1.3 AU. Thirdly, we explore and discuss the effects of these processes on the magnetic field line draping, ionisation rates, and composition in the context of the Rosetta mission. Methods. We used a new quasi-neutral hybrid model, originally designed for weakly magnetised planetary bodies, such as Venus, Mars, and Titan, and adapted here to comets. Ionisation processes were monitored individually and together following a probabilistic interaction scheme. Three-dimensional paraboloid fits of the bow shock surface, identified for a magnetosonic Mach number equal to 2, and of the cometopause surface, were performed for a more quantitative analysis. Results. We show that charge exchange and electron ionisation play a major role in the formation of a bow shock-like structure far upstream, while photoionisation is the main driver at and below the cometopause boundary, within 1000 km cometocentric distance. Charge exchange contributes to 42% of the total production rate in the simulation box, whereas production rates from electron ionisation and photoionisation reach 33% and 25%, respectively. We also discuss implications for Rosetta's observations, regarding the detection of the bow shock and the cometopause.

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A new 3‐D spherical hybrid model for solar wind interaction studies

Cited by 11 publications

References 31 publications

Mars‐solar wind interaction: LatHyS, an improved parallel 3‐D multispecies hybrid model

Mars‐solar wind interaction: LatHyS, an improved parallel 3‐D multispecies hybrid model

3D Space‐Time Adaptive Hybrid Simulations of Magnetosheath High‐Speed Jets

Hybrid modelling of cometary plasma environments

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