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Here is a fascinating text that integrates topics pertaining to all scales of the MHD-waves, emphasizing the linkages between the ULF-waves below the ionosphere on the ground and magnetospheric MHD-waves. It will be most helpful to graduate and post-graduate students, familiar with advanced calculus, who study the science of MHD-waves in the magnetosphere and ionosphere. The book deals with Ultra-Low-Frequency (ULF)-electromagnetic waves observed on the Earth and in Space.
The topics of investigation are divided into four general categories: (a) cavity modes of the magnetosphere resulting in the discrete spectrum of the resonant ultralow frequency waves; (b) a hydromagnetic code for the numerical study of the coupling of hydromagnetic waves in the dipole model of the magnetosphere; a theoretical model developed for explaining the phenomenon of plasma line over shoot observed in the ionospheric HF heating experiments; and thermal flamentation instability as the mechanism for generation of large scale field aligned ionospheric irregularities. For the first two topics, the hydromagnetic wave equations are analyzed analytically in cylindrical model of the magnetosphere and numerically in dipole model of the magnetosphere, respectively. While the steady state eigenvalue problem is studied in the first topic, the second topic is generalized to the boundary value problem considering the coupling between hydromagnetic waves in the realistic geometry of the magnetosphere. For the third topic, a nonlinear turbulent theory (resonance instability excited by a powerful high frequency in the ionosphere. For the last topic, the thermal nonlinearity gives rise to the mode-mode coupling; threshold field and the growth rate of the instability are derived. (jhd).
Perturbation electric and magnetic fields carry in excess of 10(exp10) to 10(exp12) W of electrical power between the magnetosphere and high-latitude ionosphere. Most of this power is generated by the solar wind. The ionosphere at large spatial and temporal scales acts as a dissipative slab which can be characterized by its height-integrated Pedersen conductivity sigma p, so that the power flux into the ionosphere due to a quasi-static electric field E is given by sigma (pE2) The energy transferred to the ionosphere by time-varying electromagnetic fields in the form of Alfven waves is more difficult to calculate because density and conductivity gradients can reflect energy. Thus, field resonances and standing wave patterns affect the magnitude and altitude distribution of electrical energy dissipation. We use a numerical model to calculate the frequency-dependent electric field reflection coefficient of the ionosphere and show that the ionosphere does not behave as a simple resistive slab for electric field time scales less than a few seconds. Time variation of spacecraft-measured high-latitude electric and perturbation magnetic fields is difficult to distinguish from spatial structuring that has been Doppler-shifted to a non-zero frequency in the spacecraft frame. However, by calculating the frequency-dependent amplitude and phase relations between fluctuating electric and magnetic fields we are able to show that low frequency fields (
The reduction of the oscillations of the magnetosphere to a simple mechanical analogue, which can be analyzed in detail, is accomplished in three stages: (1) The comparison of the wave equations for a dipole field magnetized plasma to those for a rectangular model of the plasmasphere with a unidirectional field -- the important physical characteristics are shown to be independent of the particular geometry chosen; (2) the comparison of the equations in the above hydromagnetic box with those of a mechanical system consisting of a set of oscillators, representing field lines, coupled by a wave propagating medium -- for the symmetric modes with weak ion-cyclotron coupling, the equations for the hydromagnetic and mechanical systems are essentially identical; (3) the simplification of the mechanical system to an elementary wave-oscillator model representing the coupling between resonant poloidal and toroidal modes -- the nature of the motion of this model is independent of the strength of the coupling. In general, the behavior of coupled and uncoupled modes is essentially different. When any coupling is present, steady state solutions, as normally understood, are not possible. (Author).
Solar-terrestrial physics deals with phenomena in the region of space between the surface of the Sun and the upper atmosphere of the Earth, a region dominated by matter in a plasma state. This area of physics describes processes that generate the solar wind, the physics of geospace and the Earth's magnetosphere, and the interaction of magnetospheri