Formation and evolution of flapping and ballooning waves in magnetospheric plasma sheet

John, Z. G.; Hirose, Akira

doi:10.1134/s1063780x16050093

Cited by 3 publications

(2 citation statements)

References 58 publications

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“…Rather, it develops due to the coupling between the Alfvén and drift compressional modes in inhomogeneous plasma. This instability can be responsible for the generation of the azimuthal small scale ULF waves in the magnetosophere, such as compressional Pc5 pulsations [32,33] as well as various kinds of the near magnetotail's perturbations [17,34,35].…”

Section: Discussionmentioning

confidence: 99%

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Non-resonant instability of coupled Alfvén and drift compressional modes in magnetospheric plasma

Mager

Klimushkin

2017

Plasma Phys. Control. Fusion

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A new mechanism of generation of the high-m compressional ULF waves in the magnetosphere is considered. It is suggested that the wave can be generated by the non-resonant instability of coupled Alfvén and drift compressional modes in the energetic component of the magnetospheric plasma. A stability analysis of the of the coupled modes in the inhomogeneous finite-β plasma in the dipole-like field in gyrokinetics is performed. A quadratic equation was obtained that determines mode frequency and the growth rate. The frequencies of both modes depend on the azimuthal wave number, m. The branches are merged at some critical m value, forming a mode with both real and imaginary parts of the wave frequency. This mode is amplified due to the instability called the drift coupling instability. The instability criterion was found. Its growth rate is determined by the mode coupling.

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Section: Discussionmentioning

confidence: 99%

“…Another ULF wave's branch that can exist in the space plasmas is the drift compressional mode [13,14]. This mode can be responsible for the so-called 'compressional storm time Pc5 pulsations' [15,16] and the flapping waves in the magnetotail [17]. Observational evidences for these modes were obtained in recent radar studies [18][19][20].…”

Section: Introductionmentioning

confidence: 97%

Non-resonant instability of coupled Alfvén and drift compressional modes in magnetospheric plasma

Mager

Klimushkin

2017

Plasma Phys. Control. Fusion

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On physical optics approximation of stratified shear flows with eddy viscosity

Karjanto

2021

Physics of Fluids

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We study a mathematical model of a perturbed stratified shear mean flow in the presence of eddy coefficients of turbulent viscosity. We adopt the standard Boussinesq approximation in the natural convection of the buoyancy-driven flow and neglect the influence of the eddy coefficients of turbulent diffusivity. Comprising both the vertical and horizontal viscosity effects, a model for the vertical velocity perturbation corresponds to a fourth-order Taylor–Goldstein (TG) differential equation. Considering only the latter, we obtained a modified TG equation with the same order as the classical, inviscid one. Under an assumption of the slowly varying Brunt–Väisälä frequency and background horizontal velocity, we discuss the corresponding geometrical and physical optics approximations of the modified TG equation using the WKB method. We further investigate the behavior of these asymptotic solutions near singular values of a turning point and critical level.

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Atmospheric Layers in Response to the Propagation of Gravity Waves under Nonisothermal, Wind-shear, and Dissipative Conditions

John

2016

JMSE

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We study the atmospheric structure in response to the propagation of gravity waves under nonisothermal (nonzero vertical temperature gradient), wind-shear (nonzero vertical zonal/meridional wind speed gradients), and dissipative (nonzero molecular viscosity and thermal conduction) conditions. As an alternative to the "complex wave-frequency" model proposed by Vadas and Fritts, we employ the traditional "complex vertical wave-number" approach to solving an eighth-order complex polynomial dispersion equation. The empirical neutral atmospheric models of NRLMSISE-00 and HWM93 are employed to provide mean-field properties. In response to the propagation of gravity waves, the atmosphere is driven into three sandwich-like layers: the adiabatic layer (0-130 km), the dissipation layer (130-230 km) and the pseudo-adiabatic layer (above 230 km). In the lower layer, (extended-)Hines' mode or ordinary dissipative wave modes exist, whereas viscous dissipation and thermal conduction fail to exert perceptible influences; in the middle layer, Hines' mode ceases to exist, and both ordinary and extraordinary dissipative wave modes flourish; in the top layer, only extraordinary wave modes survive, and dissipations affect the real part of the vertical wavenumber (m r) substantially; however, they contribute little to the imaginary part, which is the vertical growth rate (m i). We also analyze the transition of Hines' classical mode to ordinary dissipative wave modes, describe both the upward and downward modes of gravity waves and illustrate nonisothermal and wind-shear effects on the propagation of gravity waves of different modes.

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Formation and evolution of flapping and ballooning waves in magnetospheric plasma sheet

Cited by 3 publications

References 58 publications

Non-resonant instability of coupled Alfvén and drift compressional modes in magnetospheric plasma

Non-resonant instability of coupled Alfvén and drift compressional modes in magnetospheric plasma

On physical optics approximation of stratified shear flows with eddy viscosity

Atmospheric Layers in Response to the Propagation of Gravity Waves under Nonisothermal, Wind-shear, and Dissipative Conditions

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