To the Interchange Instability Criterion in the Magnetosphere in the Presence of Velocity Shear

Khazanov, G. V.; Krivorutsky, Emanuel N.; Chen, Margaret W.; Lemon, C.

doi:10.1029/2020ja028172

Cited by 3 publications

(3 citation statements)

References 22 publications

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“…Many space physicists have discussed ballooning and interchange (e.g. Panov et al (2022); Khazanov et al (2020); Sorathia et al (2020); Southwood and Kivelson (1989); Mazur et al (2013); Liu (1997); Cowley et al (2015); Schindler and Birn (2004); Pritchett and Coroniti (2010); Birn et al (2011)). In our definition, ballooning is a much more general phenomenon than interchange.…”

Section: Introductionmentioning

confidence: 99%

“…In this paper, we consider wave motion as being confined to the xz plane. The case in which the gradient is not on a plane has been considered theoretically (Xing & Wolf, 2007;Khazanov et al, 2020) but the results conflict, and the situation has not been resolved. Section 2 of the paper uses analytic theory and the energy principle to derive formulas for the eigenfunctions and eigenfrequencies within the classic interchange theory.…”

Section: Introductionmentioning

confidence: 99%

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Pure Interchange Oscillations of Thin Filaments in an Average Magnetosphere

Toffoletto¹,

Wolf²,

Derr³

2022

Preprint

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Pure Interchange Oscillations of Thin Filaments in an Average Magnetosphere

Toffoletto¹,

Wolf²,

Derr³

2022

Preprint

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“…Many space physicists have discussed ballooning and interchange oscillation modes (e.g., Agapitov et al., 2008; Birn et al., 2011; Cheremnykh & Parnowski, 2004, 2006; Cowley et al., 2015; Khazanov et al., 2020; Liu, 1997; Mazur et al., 2013; Ohtani et al., 1989a, 1989b; Pritchett & Coroniti, 2010; Schindler & Birn, 2004; Southwood & Kivelson, 1989; Sorathia et al., 2020; Panov et al., 2022). In our definition, ballooning is a much more general phenomenon than interchange.…”

Section: Introductionmentioning

confidence: 99%

Thin Filaments in an Average Magnetosphere: Pure Interchange Versus Ballooning Oscillations

2022

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This paper explores the relationship between two kinds of linear MHD disturbances, namely interchange and ideal magnetohydrodynamic (MHD) ballooning. We consider the limit of zero ionospheric conductance (see Appendix A). In that case, the square of the frequency ω 2 is real. If ω 2 > 0, it represents a wave, and ω 2 < 0, it represents a instability. In this paper, we are mostly concerned with waves. For simplicity, we consider even waves with k ‖ ∼ 0 propagating in the meridional xz plane (An even wave is one in which the perpendicular displacement is symmetric about the equatorial plane.). We define k ‖ := 2π/λ, where λ is the wavelength of the thin filament mode. Our (x, y, z)-coordinates are the geocentric solar magnetospheric (GSM) coordinate system. We consider waves in thin magnetic filaments, which have been studied in various geometries [e.g., solar corona (Parker, 1981); and magnetosphere (Chen & Wolf, 1999;Toffoletto et al., 2020;Wolf et al., 2012)]. These structures are infinitesimally thin in the y-direction and also in the xz plane perpendicular to the magnetic field. They slide through the magnetospheric background without friction. In a uniform medium, there are three MHD wave modes (fast, intermediate, and slow). The fast modes do not propagate in thin filaments (Chen & Wolf, 1999). We

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MMS Observations of Electron Vorticity in the Earth’s Magnetosheath

Li,

Yuan,

Huang

et al. 2024

ApJ

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The Earth’s magnetosheath serves as a natural laboratory to study the transition of highly turbulent fluctuations. The fundamental information about plasma turbulences can be examined observationally with the help of electron vorticity measurements. This study presents the first statistics of the electron vorticity field in the magnetosheath by utilizing 4 yr data from NASA’s Magnetospheric Multiscale mission. In this study, the magnetosheath vorticity has a dominant perpendicular anisotropy. The vorticity field in the subsolar region is much stronger than that of magnetosheath flanks. Clear dusk-favored asymmetry for large vorticity is identified in the subsolar region. We examine that the electron flow vorticity in the turbulent magnetosheath is well anticorrelated with the electron density. The vorticity is of great importance in energy dissipation and electron heating in the magnetosheath flanks. This study can improve the current understanding of electron vorticity due to its ubiquitous role in space plasma turbulences.

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To the Interchange Instability Criterion in the Magnetosphere in the Presence of Velocity Shear

Cited by 3 publications

References 22 publications

Pure Interchange Oscillations of Thin Filaments in an Average Magnetosphere

Pure Interchange Oscillations of Thin Filaments in an Average Magnetosphere

Thin Filaments in an Average Magnetosphere: Pure Interchange Versus Ballooning Oscillations

MMS Observations of Electron Vorticity in the Earth’s Magnetosheath

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