Titlebook: Magnetospheric Physics; Proceedings of the A B. M. McCormac Conference proceedings 1974 D. Reidel Publishing Company, Dordrecht, Holland 19

尖酸一点

The Reconnecting Magnetospheretion of the magneto-pause is too small to generate any magnetospheric dynamo effect of consequence. In the latter the net crossing flux is sufficient to account directly for such observed effects. Open models require field reconnection, closed ones do not. In ideal closed models no flux whatsoever c

BARK

Neutral Line in the Magnetotailil as a consequence of the reconnection process operating on the dayside magnetopause (Dungey, 1963). In order that the flux content of the tail does not grow indefinitely it is required that the reconnection process operates also in the magnetotail and allows the field lines to return to the daysid

杀虫剂

sterilization

On the Topology of the Geomagnetic Fieldcal considerations of the solar wind interaction with the geomagnetic field, the topology of the magnetosphere is fairly well understood now, at least in as much as the quiet time macroscopic structure is concerned (e.g., reviews by Ness, 1969, 1972; Fairfield, 1970; Cain, 1971; Sugiura, 1971).

Preserve

低位的人或事

Theory of the Jovian Radiation Beltsnd decimetric emissions and theoretical concepts, most of which were developed for the terrestrial magnetosphere. Since the terrestrial magnetosphere and radiation belts are far from being understood, a number of surprises can be expected from space missions to Jupiter on Pioneer 10 and 11 and Marin

展览

agitate

The Pitch Angle Distribution of > 40 keV Electronseractions and instabilities that have been discussed in the literature those dealing with gyro-resonant interactions have received considerable attention. A recent review by Gendrin (1972) on these types of wave-particle interactions summarizes the present state of the theories and points out that “

extrovert

Pitch Angle Diffusion of Relativistic Electrons in the Plasmasphereon coefficient can be radically different from the instantaneous diffusion coefficient since electrons both bounce and drift average the waves. Analysis of the time evolution of the 1.2 and 2.1 MeV electron pitch angle distributions following the October 28 and November 1, 1962, Russian high altitud

滴注

Dependent Peaks in the Energy Spectra of Electrons Precipitating from the Inner Belthe inner radiation belt (Imhof .., 1973). The energies of the peaks in the . shell interval ~ 1.4 to ~ 1.8 at .. < 0 often decrease very rapidly with increasing . value. This paper complements the previous study by presenting some new data on the distributions in energy of the peaks at a given . val