Excitation of a magnetospheric MHD cavity by Kelvin-Helmholtz instability

Mazur, V. A.; Chuiko, D. A.

doi:10.1134/s1063780x11090121

Cited by 16 publications

(16 citation statements)

References 10 publications

Supporting

Mentioning

Contrasting

Unclassified

Order By: Relevance

“…by Kelvin-Helmholtz or Kruskal-Schwarzschild instability (e.g. Mishin, 1993;Fujita et al, 1996;Plaschke and Glassmeier, 2011;Mazur and Chuiko, 2011).…”

Section: Introductionmentioning

confidence: 99%

Spatio-temporal structure of Alfvén waves excited by a sudden impulse localized on an L-shell

Klimushkin

Mager

Glassmeier³

2012

Ann. Geophys.

View full text Add to dashboard Cite

Abstract. This paper is concerned with the spatial structure and temporal evolution of the azimuthally small scale Alfvén wave generated by a sudden impulse concentrated on a given magnetic shell. At the outset, both poloidal and toroidal components are present in the wave's magnetic field. The oscillation in the poloidal component on a given magnetic shell is a superposition of two monochromatic oscillations, one with the local resonance frequency on this shell, and the other with the frequency corresponding to the resonance frequency on the source surface. The superposition of these two oscillations leads to beating. Due to phase mixing, the poloidal component of the oscillation decreases with time down to zero, transferring its energy to the toroidal component. Beating in the toroidal component is less pronounced. As time elapses, energy concentration near the source magnetic shell occurs with the frequency of the oscillation corresponding to the Alfvénic resonance frequency on this surface. Outside this thin region wave amplitudes become rather small at oscillation frequencies corresponding to the local resonance frequency of the respective magnetic shell.

show abstract

“…by Kelvin-Helmholtz or Kruskal-Schwarzschild instability (e.g. Mishin, 1993;Fujita et al, 1996;Plaschke and Glassmeier, 2011;Mazur and Chuiko, 2011).…”

Section: Introductionmentioning

confidence: 99%

Spatio-temporal structure of Alfvén waves excited by a sudden impulse localized on an L-shell

Klimushkin

Mager

Glassmeier³

2012

Ann. Geophys.

View full text Add to dashboard Cite

show abstract

“…In this case, a natural problem of determining the eigen oscillations of the system under consideration and their corresponding eigenfrequencies ω = ω ( k y , k z ) and eigenfunctions ξ x = ξ x ( x , k y , k z ) arises. Exactly, such a problem was solved in Mazur and Chuiko [, ].…”

Section: Results Of One‐dimensional Modelmentioning

confidence: 99%

“…A plot of the real part of the frequency as a function of the solar wind speed V is shown in Figure c for one of the modes of the magnetosphere‐solar wind system [ Mazur and Chuiko , ]. This plot reflects the α ≠ 0, δ A = 0 case, for simplicity.…”

Section: Results Of One‐dimensional Modelmentioning

confidence: 99%

“…Therefore, the results obtained for a one‐dimensional inhomogeneous medium (inhomogeneous over x but homogeneous over y ) are very important for describing oscillations of a two‐dimensional inhomogeneous medium. Our recent studies [ Mazur and Chuiko , , ] were dedicated to investigation of this subject. In the next section, we give a short review of the results of those studies.…”

Section: Model Of Medium and Wkb Approximation Along Azimuthmentioning

confidence: 99%

See 1 more Smart Citation

Azimuthal inhomogeneity in the MHD waveguide in the outer magnetosphere

Mazur

Chuiko

2015

JGR Space Physics

Self Cite

View full text Add to dashboard Cite

Geomagnetic field and plasma inhomogeneities in the outer equatorial part of the magnetosphere create a channel with low Alfvén speeds which spans from the nose to the far flanks of the magnetosphere, in both the morning and the evening sectors. This channel plays the role of a waveguide for fast magnetosonic waves. The waveguide eigenmodes and corresponding Alfvén resonance (field line resonance) regions are directly related to geomagnetic pulsations Pc3 and Pc5. U-shaped model of the waveguide allows for full analytical investigation of waveguide eigenmodes. Quantities such as mode wave numbers, group velocities, and their energy density distribution are found as functions of coordinate along the waveguide. The linkage of the waveguide magnetosonic oscillation energy to the Alfvén waves in the vicinity of the field line resonance deeper inside the magnetosphere is investigated, and corresponding energy leakage coefficient is found. Thus, the influence of longitudinal (i.e., azimuthal) waveguide inhomogeneity on wave propagation is analytically investigated. Obtained results can be used for interpretation of the observed wave power distribution in the frequency bands of geomagnetic pulsations Pc3 and Pc5, as well as for explanation of their spectral properties in the outer magnetosphere.

show abstract

“…Theoretical investigations assume that the magnetopause transition layer is unstable to fast magnetosonic (FMS) waves (Cheremnykh et al., ; Pu & Kivelson, ). There are three types of FMS oscillations excited by the KH instability at the magnetopause (Leonovich & Kozlov, ): surface waves propagating along the magnetopause, for which both the solar wind and magnetosphere are opacity regions; radiative modes (FMS waves emitted by the magnetopause into the solar wind, if it is a transparency region for them); and the eigenmodes of the FMS resonator (or waveguide) formed by the magnetopause and the turning surfaces separating the transparency and opacity regions in the magnetosphere and/or in the solar wind (Mazur & Chuiko, , ).…”

Section: Introductionmentioning

confidence: 99%

Kelvin‐Helmholtz Instability in a Dipole Magnetosphere: The Magnetopause as a Tangential Discontinuity

Leonovich

Козлов

2019

JGR Space Physics

View full text Add to dashboard Cite

The boundary stability problem is solved for a dipole magnetosphere wrapped by an azimuthal solar wind flow. A simplified equation is obtained describing small‐scale fast magnetosonic waves in a dipole magnetosphere. The structure of surface fast magnetosonic waves along magnetic field lines is represented as an expansion into a set of standing (between the magnetoconjugate ionospheres) waves. Over the azimuthal coordinate, along which the plasma is homogeneous, the wave field is decomposed into a set of azimuthal harmonics. It is shown that, in solar wind flows with velocities actually observable near the Earth's magnetosphere, only surface waves corresponding to several first harmonics of these expansions are unstable. The frequency ranges of unstable oscillations do not overlap for harmonics with different wave numbers. As the plasma flow velocity increases, harmonics with higher and higher wave numbers become unstable. The characteristic frequencies of unstable surface waves cover the lowest‐frequency, Pc5–Pc6 range of geomagnetic pulsations observed in the magnetosphere. The frequency spectrum of these oscillations corresponds to geomagnetic pulsations at discrete “magic frequencies” occasionally observed in the Earth's magnetosphere.

show abstract

Excitation of a magnetospheric MHD cavity by Kelvin-Helmholtz instability

Cited by 16 publications

References 10 publications

Spatio-temporal structure of Alfvén waves excited by a sudden impulse localized on an L-shell

Spatio-temporal structure of Alfvén waves excited by a sudden impulse localized on an L-shell

Azimuthal inhomogeneity in the MHD waveguide in the outer magnetosphere

Kelvin‐Helmholtz Instability in a Dipole Magnetosphere: The Magnetopause as a Tangential Discontinuity

Contact Info

Product

Resources

About