Formation, spin-up, and stability of field-reversed configurations

Omelchenko, Y. A.

doi:10.1103/physreve.92.023105

Cited by 11 publications

(10 citation statements)

References 18 publications

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“…The Chodura resistivity has been employed in simulations of reconnection in fieldreversed configurations, showing agreement with experiments (e.g., Omelchenko [2015]; Kayama, [2012]). We have benchmarked our resistivity model against full particle-in-cell simulations of established configurations [e.g., Chen et al, 2012] and reproduced electron-scale reconnecting current sheets.…”

Section: The Global Hybrid Simulationmentioning

confidence: 53%

“…Our hybrid simulation imposes the Chodura resistivity (e.g., Milroy & Brackbill, 1982;Sgro & Nielson, 1976), a semiempirical model with dependence on the current density and number density. The Chodura resistivity has been employed in simulations of reconnection in field-reversed configurations, showing agreement with experiments (e.g., Kayama, 2012;Omelchenko, 2015). We have benchmarked our resistivity model against full particle-in-cell simulations of established configurations (e.g., Chen et al, 2012) and reproduced electron-scale reconnecting current sheets.…”

Section: The Global Hybrid Simulationmentioning

confidence: 59%

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Magnetopause Reconnection and Indents Induced by Foreshock Turbulence

Chen

Omelchenko

et al. 2021

Geophysical Research Letters

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Magnetopause reconnection plays a critical role in controlling energy input from the solar wind to the magnetosphere. The possibility that magnetic fluctuations generated in the foreshock may lead to magnetopause reconnection has been considered based on observations indicating that magnetosheath fields are not a simple compression of the interplanetary magnetic field (IMF) (Russell et al., 1997;Zhang et al., 1997). On account of the fact that the statistical magnetopause locations for cone angles (between the IMF and the Sun-Earth line) greater and less than 45° do not differ appreciably, the study by Zhang et al. (1997) concludes that the raised possibility is not confirmed. Recent measurements from the Magnetospheric Multiscale mission show Earth-radius-scale foreshock magnetic and density fluctuations approximately one order of magnitude larger than the respective upstream values under quasi-radial IMF (cone angles <30°) conditions (Chen et al., 2021). These intense fluctuations often contain strong B z (in Geocentric Solar magnetic (GSM) coordinates) and B y components. If these fluctuations can reach the magnetopause, they can create conditions conducive to reconnection. In this paper, based on global hybrid simulation results, we predict that foreshock fluctuations in the form of strong B z and density fluctuations can reach the magnetopause and lead to reconnection as well as Earth-sized indents.To single out the effects of foreshock fluctuations, we design our simulation to have a quasi-radial IMF with a weak northward (B z > 0) and zero dawn-dusk (B y = 0) components. When the IMF is quasi-radial, foreshock waves excited due to reflected ions interacting with the incoming solar wind are the strongest, permeate the largest volume of the subsolar region, and can most strongly influence the inner magnetosphere (e.g., Russell et al.,1983; Takahashi et al., 2021, and references therein). In the aspect of reconnection, extensive statistical studies show that magnetopause reconnection occurs for shear angles (angle between the magnetosheath and magnetosphere magnetic fields across the magnetopause) as low as ∼30° but not lower than that (e.g.,

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Section: The Global Hybrid Simulationmentioning

confidence: 53%

Section: The Global Hybrid Simulationmentioning

confidence: 59%

Magnetopause Reconnection and Indents Induced by Foreshock Turbulence

Chen

Omelchenko

et al. 2021

Geophysical Research Letters

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“…The Chodura resistivity, η ch was previously used in 3D HYPERS simulations of field-reversed configurations (Omelchenko, 2015). The "vacuum" resistivity, η v vanishes at cells occupied with plasma, n e ≫ n min .…”

Section: Hybrid Equationsmentioning

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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“…η ch is the Chodura resistivity, which is an empirical expression previously used to model field‐reversed configurations (Y. A. Omelchenko, 2015 ). The “vacuum resistivity” η v vanishes at cells occupied with plasma.…”

Section: Simulation Modelmentioning

confidence: 99%