By Isaac Asimov

Strains the background of the research of early guy and explains what this learn has published approximately his roots.

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42) 0 where n is the unit vector perpendicular to the shock surface. Integrating of Eq. 43) One more boundary equation describes the energy balance at the bow shock. We refer the reader to Akasofu and Chapman (1972) and Landau and Lifshitz (1982) for a more complete treatise on the boundary conditions on the bow shock. To study the magnetic field at the bow shock in a little more detail, it is necessary at this point to consider the electric current flowing in the vicinity of the shock. Taking the cross product of Eq.

The region of the current inflow and issue produces practically continuous strip along the auroral oval, which results from the plasma sheet and polar cusp mapping to the high-latitude ionosphere (100–200 km over the Earth surface). In this region the aurora borealism and magnetic storms are frequently observed due to the energetic particles precipitating along field lines from the magnetosphere into the ionosphere. The plasmasphere is the region, which contains the ionospheric plasma with enhanced number density n 103 cm 3 and thermal energy 1:0 eV.

Similarly, in the first approximation Eq. 49) 0 To simplify the problem, we assume that the fluid conductivity ! 1, so that the magnetic field lines are frozen into the conducting fluid. This means that the electric field can be derivable from the velocity through Eq. 35), that is E D B0 V. In such a case Eq. @P =@ /S is the squared sound velocity taken at the constant entropy. We seek for the solution of the set of Eqs. 51) in the form of harmonic wave. t /, where k is the wave vector and ! is the frequency.

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