Generation and propagation of the ULF planetary-scale electromagnetic wavy structures in the ionosphere

Aburjania, G. D.; Chargazia, Kh. Z.; Jandieri, G. V.; Khantadze, A. G.; Kharshiladze, O.; Lominadze, J. G.

doi:10.1016/j.pss.2005.02.004

Cited by 21 publications

(29 citation statements)

References 32 publications

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“…The errors made by assuming that the magnetic and rotation axes coincide is of the same order as the errors inherent in the β-plane approximation (see e.g. Aburjania et al, 2005;Kaladze et al, 2003). For the above scales of disturbances, the consequences of the misalignment of both axes, which is about 0.2 rad, are beyond the accuracy of the β-plane approximation and, therefore, cannot change the results qualitatively.…”

Section: Yu Rapoport Et Al: Excitation Of Planetary Electromagneticmentioning

confidence: 96%

“…Herron (1966) has found that these waves can be captured into the ionospheric waveguide at the Alfvén speed minimum in the F region. Further development of these ideas brought the concept of vortex planetary electromagnetic waves (Kaladze et al, 2003;Khantadze, 1973;Aburjania et al, 2002Aburjania et al, , 2003aAburjania et al, , 2005Aburjania and Chargazia, 2011;Rapoport et al, 2011Rapoport et al, , 2012c. The developed theory of PEMW is supported by a number of observational results of planetary-scale electromagnetic perturbations (see e.g.…”

Section: Introduction and Formulation Of The Problemmentioning

confidence: 99%

“…The nonlinear system of equations for PEMW, valid for any height, from D to F regions, including intermediate altitudes between D and E and between E and F regions, is derived. In particular, we have found the system of nonlinear one-fluid MHD equations in the β-plane approximation valid for the ionospheric F region (Aburjania et al, 2003a(Aburjania et al, , 2005. The series expansion in a "small" (relative to the local geomagnetic field) non-stationary magnetic field has been applied only at the last step of the derivation of the equations.…”

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confidence: 99%

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Excitation of planetary electromagnetic waves in the inhomogeneous ionosphere

et al. 2014

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Abstract. In this paper we develop a new method for the analysis of excitation and propagation of planetary electromagnetic waves (PEMW) in the ionosphere of the Earth. The nonlinear system of equations for PEMW, valid for any height, from D to F regions, including intermediate altitudes between D and E and between E and F regions, is derived. In particular, we have found the system of nonlinear one-fluid MHD equations in the β-plane approximation valid for the ionospheric F region (Aburjania et al., 2003a(Aburjania et al., , 2005. The series expansion in a "small" (relative to the local geomagnetic field) non-stationary magnetic field has been applied only at the last step of the derivation of the equations. The small mechanical vertical displacement of the media is taken into account. We have shown that obtained equations can be reduced to the well-known system with Larichev-Reznik vortex solution in the equatorial region (see e.g. Aburjania et al., 2002). The excitation of planetary electromagnetic waves by different initial perturbations has been investigated numerically. Some means for the PEMW detection and data processing are discussed.

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Section: Yu Rapoport Et Al: Excitation Of Planetary Electromagneticmentioning

confidence: 96%

Section: Introduction and Formulation Of The Problemmentioning

confidence: 99%

mentioning

confidence: 99%

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Excitation of planetary electromagnetic waves in the inhomogeneous ionosphere

et al. 2014

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“…where From the expressions (11)- (13) follow that the phase speed of fast planetary waves (formula (11)) does not depend on the wave number, do not experience dispersion and they propagate one-dimensional, however slow Rossby type waves in E region and fast waves in F region of the ionosphere are strongly dispersive. The considered waves have all-planetary character and they can be exited at all latitudes of Earth.…”

Section: Dispersian Equations and Estimation Of The Wave Parameters Fmentioning

confidence: 99%

“…These waves in [8,9] were called magnetogradient waves of Khantadze. In the above-stated papers [2][3][4][5][6][7] classification of magnetogradient planetary waves (fast and slow), hydrodynamic end electromagnetic nature of these waves and the anisotropic nature of their propagation caused by curvature of lines of force of the geomagnetic field along the Earth parallels was for the first time given. Assessment of parameters of the considered waves, and also linear and nonlinear theories of magnetogradient waves, is given in [10][11][12][13][14]. Experimentally these waves were recorded in [8,15,16].…”

Section: Introductionmentioning

confidence: 99%

Three-Dimensional Magnetogradient Waves in the Upper Atmosphere

Jandieri

Gvelesiani

Diasamidze

et al. 2017

JAP

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I S S N 2347-3487 V o l u m e 1 3 N u m b e r 5 J o u r n a l o f A d v a n c e s i n P h y s i c s | THREE-DIMENSIONAL MAGNETOGRADIENT WAVES IN THE UPPER ATMOSPHERE ABSTRACTGeneral dispersion equation has been obtained for three-dimensional electromagnetic planetary waves, from which follows, as particular case Khantadze results in one-dimension case. It was shown that partial magnetic field line freezingin as in one-dimension case lead to the excitation of both "fast" and "slow" planetary waves, in two-liquid approximation (i.e. at ion drag by neutral particles) they are represent oscillations of magnetized electrons and partially magnetized ions in E region of the ionosphere. In F region of the ionosphere using one-liquid approximation only "fast" planetary wave will be generated representing oscillation of medium as a whole. Hence, it was shown that three-dimension magnetogradient planetary waves are exist in all components of the ionosphere, and as exact solutions, with well-known slow short-wave MHD waves, are simple mathematical consequence of the MHD equations for the ionosphere.

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Magnetic Turbulence in the Geospace Environment

et al. 2010

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Magnetic turbulence is found in most space plasmas, including the Earth's magnetosphere, and the interaction region between the magnetosphere and the solar wind. Recent spacecraft observations of magnetic turbulence in the ion foreshock, in the magnetosheath, in the polar cusp regions, in the magnetotail, and in the high latitude ionosphere are reviewed. It is found that: 1. A large share of magnetic turbulence in the geospace environment is generated locally, as due for instance to the reflected ion beams in the ion foreshock, to temperature anisotropy in the magnetosheath and the polar cusp regions, to velocity shear in the magnetosheath and magnetotail, and to magnetic reconnection at the magnetopause and in the magnetotail. 2. Spectral indices close to the Kolmogorov value can be recovered for low frequency turbulence when long enough intervals at relatively constant flow speed are analyzed in the magnetotail, or when fluctuations in the magnetosheath are G. Zimbardo et al. considered far downstream from the bow shock. 3. For high frequency turbulence, a spectral index α 2.3 or larger is observed in most geospace regions, in agreement with what is observed in the solar wind. 4. More studies are needed to gain an understanding of turbulence dissipation in the geospace environment, also keeping in mind that the strong temperature anisotropies which are observed show that wave particle interactions can be a source of wave emission rather than of turbulence dissipation. 5. Several spacecraft observations show the existence of vortices in the magnetosheath, on the magnetopause, in the magnetotail, and in the ionosphere, so that they may have a primary role in the turbulent injection and evolution. The influence of such a turbulence on the plasma transport, dynamics, and energization will be described, also using the results of numerical simulations.

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Generation and propagation of the ULF planetary-scale electromagnetic wavy structures in the ionosphere

Cited by 21 publications

References 32 publications

Excitation of planetary electromagnetic waves in the inhomogeneous ionosphere

Excitation of planetary electromagnetic waves in the inhomogeneous ionosphere

Three-Dimensional Magnetogradient Waves in the Upper Atmosphere

Magnetic Turbulence in the Geospace Environment

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