Comparison Between Fluid Simulation With Test Particles and Hybrid Simulation for the Kelvin‐Helmholtz Instability

Ma, Xuanye; Delamere, P. A.; Nykyri, K.; Burkholder, Brandon; Neupane, B. R.; Rice, Rachel

doi:10.1029/2019ja026890

Cited by 14 publications

(24 citation statements)

References 56 publications

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“…It should be noted that magnetic reconnection is prevalent in the KH instability (Ma et al, 2017). In two-dimensional simulation studies, Ma et al (2019) found that mass transport in MHD simulations is facilitated by magnetic reconnection, while in hybrid simulations the transport DELAMERE ET AL.…”

Section: Resultsmentioning

confidence: 99%

Kelvin–Helmholtz‐Related Turbulent Heating at Saturn's Magnetopause Boundary

Delamere

Damiano

et al. 2021

JGR Space Physics

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One of the grand challenge problems of the giant planet magnetospheres is the issue of nonadiabatic plasma heating. Simple turbulent heating models consider the energy cascade rate from one scale to another where the energy density is based on perpendicular magnetic fluctuations of counterpropagating Alfvén waves. Analytical expressions from turbulence theory for the heating rate density have yielded promising results for the observed ion heating at Jupiter and Saturn. Here, we compare ion heating using hybrid simulations of the Kelvin–Helmholtz instability and analytical estimates in an effort to validate turbulence theory and further understand the nature of the ion heating. Heating rate densities ∼10−15 W/m3 are produced in our three‐dimensional Kelvin–Helmholtz simulations during the nonlinear growth phase and compare favorably with analytical estimates. Results targeting Saturn will be discussed in the broader context of radial plasma transport in the rapidly rotating magnetospheres.

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Section: Resultsmentioning

confidence: 99%

Kelvin–Helmholtz‐Related Turbulent Heating at Saturn's Magnetopause Boundary

Delamere

Damiano

et al. 2021

JGR Space Physics

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“…Note that the SAMU model identifies the magnetosheath and magnetosphere by using an empirical model, which can misidentify the region if the boundary is strongly modified by the local processes (e.g., magnetic reconnection and KH instability). Thus, this map may somewhat exaggerate the mixing, although several of those local processes are usually important plasma mixing mechanisms (e.g., Ma et al., 2019).…”

Section: Statistical Survey Resultsmentioning

confidence: 99%

“…Journal of Geophysical Research: Space Physics exaggerate the mixing, although several of those local processes are usually important plasma mixing mechanisms (e.g., Ma et al, 2019).…”

Section: 1029/2020ja028209mentioning

confidence: 99%

Statistical Study of Solar Wind, Magnetosheath, and Magnetotail Plasma and Field Properties: 12+ Years of THEMIS Observations and MHD Simulations

Nykyri

Dimmock

et al. 2020

JGR Space Physics

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The solar wind plasma is a major plasma source for the Earth's magnetosphere, which has a strong influence on the magnetotail plasma and field properties. The relative importance of different plasma entry mechanisms and pathways is largely determined by the solar wind conditions. Therefore, the spatial and temporal dependence of magnetotail plasma and field properties under different kinds of solar wind conditions is critically important for understanding the Earth's magnetosphere. This study presents a statistical study of fundamental magnetotail plasma properties in a normalized reference frame by utilizing 12+ years of data from NASA's Time History of Events and Macroscale Interactions during Substorms (THEMIS) mission. These statistical maps are mostly in agreement with the magnetosheath of MHD runs from the CCMC BATS-R-US model, but some features in the maps can be explained by kinetic particle physics, not present in the MHD. The results are also used to investigate the presence of any magnetotail plasma parameter asymmetries and their possible causes. Plain Language Summary Earth's intrinsic magnetic field, generated by the currents in the Earth's interior, protects our planet from solar radiation and plasma called the solar wind. However, physical processes such as magnetic reconnection occurring at the boundary of this magnetic barrier, the magnetosphere, can break this shield, enabling access of solar wind plasma into the Earth's magnetosphere. Earth's ionosphere provides another source for magnetospheric plasma. This plasma can be further accelerated to huge energies, which provides a threat for astronauts and satellites. The effectiveness of physical mechanisms that control the entry and acceleration of this plasma strongly depends on the local magnetic field geometry and plasma properties, which in turn are affected by the solar wind. However, the solar wind properties are not constant but vary as it can originate from different regions of the sun. While the magnetic field of the Sun, the interplanetary magnetic field (IMF), on average forms an "Archimedean Spiral," flapping of the heliospheric current sheet and fluctuations along field lines will make the IMF "hit" the Earth at different orientations, thus impacting the shock geometry in front of the planet, which in turn affects the downstream plasma and field properties in the turbulent boundary layer called the magnetosheath. In this paper, we have characterized the dependence of the large-scale plasma properties in the Earth's magnetosphere and magnetosheath on the solar wind and IMF conditions by using over 12 years (thus covering over one solar cycle) of data from NASA's Time History of Events and Macroscale Interactions during Substorms (THEMIS) mission.

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“…Furthermore, this high‐latitude boundary layer can also be unstable to the KHI (Hwang et al., 2012; Nykyri et al., 2020) which can also generate temperature anisotropy (Ma et al., 2019). Global 3‐D simulations addressing both the KHI and mirror mode generation remain to be developed to fully understand the coupling of these processes.…”

Section: Discussionmentioning

confidence: 99%

Magnetospheric Multiscale Observations of the Source Region of Energetic Electron Microinjections Along the Duskside, High‐Latitude Magnetopause Boundary Layer

Nykyri

Kronberg²,

Turner

et al. 2021

Geophysical Research Letters

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The present paper demonstrates the first observations by the Magnetospheric Multiscale (MMS) mission of the counter‐streaming energetic electrons and trapped energetic protons, localized in the magnetic field depressions between the mirror mode peaks, in the Earth's dusk sector high‐latitude magnetosphere. This region is characterized by high plasma beta, strong ion temperature anisotropy, and intermediate plasma density between magnetospheric and magnetosheath plasma. We show that these plasma conditions are unstable for the drift mirror instability. The counter‐streaming electron feature resembles those of the previously reported energetic electron microinjections, but without the energy‐time dispersion signature. This suggests that MMS is passing through one of the potential microinjection source regions. The energetic ion data in the present study is mainly used to estimate the scale size of the mirror mode structures.

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Comparison Between Fluid Simulation With Test Particles and Hybrid Simulation for the Kelvin‐Helmholtz Instability

Cited by 14 publications

References 56 publications

Kelvin–Helmholtz‐Related Turbulent Heating at Saturn's Magnetopause Boundary

Kelvin–Helmholtz‐Related Turbulent Heating at Saturn's Magnetopause Boundary

Statistical Study of Solar Wind, Magnetosheath, and Magnetotail Plasma and Field Properties: 12+ Years of THEMIS Observations and MHD Simulations

Magnetospheric Multiscale Observations of the Source Region of Energetic Electron Microinjections Along the Duskside, High‐Latitude Magnetopause Boundary Layer

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