Ballooning modes in the inner magnetosphere of the Earth

Cheremnykh, O. K.; Parnowski, A. S.; Burdo, O.S.

doi:10.1016/j.pss.2004.07.014

Cited by 24 publications

(21 citation statements)

References 20 publications

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“…At the same time, the mode was found to provide a growth rate which was in agreement with Pc5 measurements by both the STARE radar and Geo 2 satellite [Pokhotelov et al, 1986]. Since then, it has become the dominant candidate used to account for the instabilities leading to substorm onset and expansion [see, e.g., Lakhina et al, 1990aLakhina et al, , 1990bRoux et al, 1991;Lui, 1996;Cheng and Lui, 1998;Pritchett and Coroniti, 1999;Miura, 2000Miura, , 2001Cheremnykh et al, 2004;Lui, 2004;Chang et al, 2012].…”

Section: Introductionsupporting

confidence: 68%

Effect of heat flux on Alfvén ballooning modes in isotropic Hall‐MHD plasmas

2014

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The magnetosphere undergoes a transition from a dipole-like to taillike structure in the antisunward direction. In this region, Alfvén ballooning instability has been considered as a leading candidate to be responsible for the onset and expansion phase of observed impulsive substorms. We apply the generalized Ohm's law in isotropic Hall-MHD equations and study the effect of heat flux on the ballooning modes under substorm circumstances. The set of partial differential equations is obtained for a general ballooning dispersion relation from which all classical Alfvén waves and fundamental ballooning modes are recovered, e.g., the decoupled shear Alfvén and magnetosonic modes, the classical ballooning instability in incompressible plasmas. In the absence of the heat flux, the ballooning mode is featured by the coupling of the two modes by the superposition of the independent Hall effect and the independent plasma inhomogeneity effect. By contrast, heat flux exerts its influence on the ballooning mode by updating the coefficients of the terms in the dispersion relation. The results expose that the growth rate ( BM ) has two branches. If k p is free, one branch shifts versus , while the other branch is damped substantially by the heat flux, leading to a more stable ballooning mode; if k c is free, one branch shifts little versus , but the other one has higher BM driven by the heat flux, leading to a more unstable ballooning mode.

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Section: Introductionsupporting

confidence: 68%

Effect of heat flux on Alfvén ballooning modes in isotropic Hall‐MHD plasmas

2014

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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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“…07.002 and SMS waves in a curvilinear magnetic field (Southwood and Saunders, 1985;Walker, 1987;Cheng and Lin 1987;Ohtani et al, 1989;Klimushkin, 1998;Cheremnykh et al, 2004;Klimushkin and Mager, 2008).…”

Section: Introductionmentioning

confidence: 99%

Magnetosonic resonances in the magnetospheric plasma

Leonovich

Козлов

2013

Earth Planet Sp

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A problem of coupling between fast and slow magnetosonic waves in Earth's magnetosphere (magnetosonic resonance) is examined. Propagation both slow magnetosonic wave and Alfven wave can easily be canalized along the magnetic field line direction. The main difference between the two is that slow magnetosonic waves dissipate strongly due to their interaction with the background plasma ions, whose temperature is above the electron temperature. In Earth's magnetosphere, however, there is a region where the dissipation of slow magnetosonic waves can be weak-the inner plasmasphere. The slow magnetosonic waves generated there can be registered directly. In other regions, with strong dissipation of slow magnetosonic waves, their signature may be detected through their impact on the Alfven resonance at frequencies for which the resonant Alfven and slow magnetosonic waves exist simultaneously in the magnetosphere. Owing to their strong coupling with the background plasma ions, resonant slow magnetosonic waves can transfer the energy and impulse from the solar wind to the magnetospheric plasma ions via fast magnetosonic waves penetrating into the tail lobes. A problem of resonant conversion of fast magnetosonic waves into slow magnetosonic oscillations in a magnetosphere with dipole-like magnetic field is also examined.

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Ballooning modes in the inner magnetosphere of the Earth

Cited by 24 publications

References 20 publications

Effect of heat flux on Alfvén ballooning modes in isotropic Hall‐MHD plasmas

Effect of heat flux on Alfvén ballooning modes in isotropic Hall‐MHD plasmas

Ballooning modes and their stability in a near-Earth plasma

Magnetosonic resonances in the magnetospheric plasma

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