Titlebook: Cosmic Plasma Physics; Proceedings of the C Karl Schindler Conference proceedings 1972 Plenum Press, New York 1972 Plasma.electron.fields.i

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书目名称Cosmic Plasma Physics影响因子(影响力)




书目名称Cosmic Plasma Physics影响因子(影响力)学科排名




书目名称Cosmic Plasma Physics网络公开度




书目名称Cosmic Plasma Physics网络公开度学科排名




书目名称Cosmic Plasma Physics被引频次




书目名称Cosmic Plasma Physics被引频次学科排名




书目名称Cosmic Plasma Physics年度引用




书目名称Cosmic Plasma Physics年度引用学科排名




书目名称Cosmic Plasma Physics读者反馈




书目名称Cosmic Plasma Physics读者反馈学科排名

maroon

Parametric Instabilities Generated in the Ionosphere by Intense Radio Wavesy. The energy content of 100 cubic kilometers of ionospheric plasma is of the order of 10 megawatt-secs. This estimate, coupled with an electron-ion temperature relaxation time ~ 10 secs, suggests the H. F. frequency transmitters in the megawatt power range can significantly alter the ionosphere pro

FOLLY

Study of a Jovian Plasmasphere and the Occurrence of Jupiter Radioburstsuence of Io on the emission of the radiobursts. Duncan (1970) proposed that Io stimulates the emission when it crosses the “magnetopause” of Jupiter, Melrose (1967) suggested that the motion of Io through a “corotating region” inside the magnetosphere of Jupiter may be the cause.

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Universal Instability Associated with the Plasmapause and Its Role in Geomagnetic Micropulsationse theory and laboratory experiments of a non-homogeneous magnetoplasma. Drift waves excited at the plasmapause may be unstable in the direction of the electron drift and propagate eastwards nearly perpendicular to the magnetic field. The drift waves, however, tend to convert very soon to ion sound o

Texture

Deformation and Striation of Barium Clouds in the Ionospherevoted to the theory of plasma clouds which are sufficiently large to dominate the Pederson conductivity on lines of force which pass through the cloud and sufficiently high so that K. = Ω./.. ≫ 1. Figure 1 shows the model.

Texture

Thermal Energy Transport in the Solar Winds with the theory for collision-dominated heat transport in a fully ionized medium developed by Spitzer and Härm [1953]. A short discussion of some recent models is included to illustrate the role of thermal conduction in the expansion. In addition, a brief description of the steady state solar wind

非实体

Influence of Neutral Interstellar Matter on the Expansion of the Solar Windially constant expansion velocity. This solution is derived from a hydrodynamical treatment of the coronal expansion that does not take into account any interaction of the solar wind plasma with neutral interstellar matter which enters the solar system. In that case the supersonic solar wind expands

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THROB

Heating of the Solar Wind Ionsn influx of neutral hydrogen from the boundary of the heliospher’e. Photoionisation and charge exchange trans-form neutral hydrogen atoms into protons. The ionised hydrogen component near the Earth’s orbit is then double-peaked and unstable. The kinetic energy of the protons (originating from the ne