Ballooning perturbations in the inner magnetosphere of the Earth: Spectrum, stability and eigenmode analysis

Agapitov, Oleksiy; Cheremnykh, O. K.; Parnowski, A. S.

doi:10.1016/j.asr.2006.12.040

Cited by 24 publications

(21 citation statements)

References 14 publications

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“…Then, in the stable case, the field lines oscillate mainly in the direction along the axis of the arcade, b r b y , while in the unstable case, they are displaced mainly in the radial direction, b r b y . This agrees with results obtained in earlier publications (Agapitov, Cheremnykh, and Parnowski, 2008;Mazur, Fedorov, and Pilipenko, 2012). Thus, the corrugation instability of an arcade distorts its boundary in the radial, i.e.…”

Section: First Equation 50supporting

confidence: 83%

“…These authors also formulated for the first time the instability criterion outside the local approximation. Cheremnykh and Parnowski (2004), Agapitov, Cheremnykh, and Parnowski (2008) and Leonovich and Kozlov (2013b) considered the instability in a plasma with an inhomogeneity along the field lines. Ma, Hirose, and Liu (2014) studied the instability in the Hall-MHD framework.…”

Section: Introductionmentioning

confidence: 99%

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Corrugation Instability of a Coronal Arcade

et al. 2017

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We analyse the behaviour of linear magnetohydrodynamic perturbations of a coronal arcade modelled by a half-cylinder with an azimuthal magnetic field and nonuniform radial profiles of the plasma pressure, temperature, and the field. Attention is paid to the perturbations with short longitudinal (in the direction along the arcade) wavelengths. The radial structure of the perturbations, either oscillatory or evanescent, is prescribed by the radial profiles of the equilibrium quantities. Conditions for the corrugation instability of the arcade are determined. It is established that the instability growth rate increases with decreases in the longitudinal wavelength and the radial wave number. In the unstable mode, the radial perturbations of the magnetic field are stronger than the longitudinal perturbations, creating an almost circularly corrugated rippling of the arcade in the longitudinal direction. For coronal conditions, the growth time of the instability is shorter than one minute, decreasing with an increase in the temperature. Implications of the developed theory for the dynamics of coronal active regions are discussed.

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Section: First Equation 50supporting

confidence: 83%

Section: Introductionmentioning

confidence: 99%

Corrugation Instability of a Coronal Arcade

et al. 2017

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“…The analysis of satellite observational data led Roux et al (1991) to the suggestion that an instability driven by the plasma pressure gradient is responsible for the field-aligned current generation during the substorm onset. Later the idea about the ballooning instability as an onset trigger has been extensively elaborated (e.g., Lee and Wolf, 1992;Liu, 1997;Cheremnykh et al, 2004;Agapitov et al, 2007).…”

Section: Introduction: Ballooning Instability Of Nearearth Plasma As mentioning

confidence: 99%

Ballooning modes and their stability in a near-Earth plasma

2013

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As a possible trigger of the substorm onset, the ballooning instability has been often suggested. The ballooning disturbances in a finite-pressure plasma immersed into a curved magnetic field are described with the system of coupled equations for the Alfven and slow magnetosonic modes. The spectral properties of ballooning disturbances and instabilities can be characterized by the local dispersion equation. The basic system of equations can be reduced to the dispersion equation for the small-scale in transverse direction disturbances. From this relationship the dispersion, instability threshold, and stop-bands of the Alfvenic and slow magnetosonic modes have been determined. The field-aligned structure of unstable mode is described with the solution of the eigenvalue problem in the Voigt model. We have also analyzed in a cylindrical geometry an eigenvalue problem for the stability of ballooning disturbances with a finite scale along the plasma inhomogeneity. The account of a finite scale in the radial direction raises the instability threshold as compared with that in the WKB approximation.

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“…As was demonstrated in Zhu et al (2004), Parnowski (2007, Agapitov et al (2008), Mazur et al (2012), and Leonovich and Kozlov (2013), the increase of the k r value deteriorates conditions for the development of the ballooning instability. As was demonstrated in Zhu et al (2004), Parnowski (2007, Agapitov et al (2008), Mazur et al (2012), and Leonovich and Kozlov (2013), the increase of the k r value deteriorates conditions for the development of the ballooning instability.…”

Section: Introductionmentioning

confidence: 79%

Ballooning Instability in the Magnetospheric Plasma: Two‐Dimensional Eigenmode Analysis

2020

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This paper is concerned with the transverse structure of the ballooning instability in a two-dimensionally inhomogeneous model of the magnetosphere, which takes into account inhomogeneity both across the magnetic shells and along the field lines. According to the previous studies, the ballooning instability can develop at steep fall of the plasma pressure from the Earth. In this paper, the region of negative plasma pressure gradient is assumed to be sharply localized across the magnetic shells. It causes the localization of the unstable perturbation in the same direction. In this region, the perturbation has a resonator-like structure, where only modes with discrete set of the growth rate values can exist. The azimuthal wave number of the unstable mode must exceed some critical value, which is determined by the width of the localization region.

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Ballooning perturbations in the inner magnetosphere of the Earth: Spectrum, stability and eigenmode analysis

Cited by 24 publications

References 14 publications

Corrugation Instability of a Coronal Arcade

Corrugation Instability of a Coronal Arcade

Ballooning modes and their stability in a near-Earth plasma

Ballooning Instability in the Magnetospheric Plasma: Two‐Dimensional Eigenmode Analysis

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