Physics
Scientific paper
Jul 1983
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983rpspr..23...55b&link_type=abstract
In its USSR Rept.: Space, No. 23 (JPRS-83994) p 55-57 (SEE N83-31617 20-12) Transl. into ENGLISH from Pravda (Moscow), 10 Jan.
Physics
Interplanetary Medium, Planetary Magnetic Fields, Planetary Magnetospheres, Radio Waves, Venus (Planet), Wave Propagation, Cosmic Plasma, Interstellar Gas, Pressure Effects, Shock Waves, Solar Wind Velocity, Venera Satellites
Scientific paper
Nonuniformity in the structure of the solar corona and the transience of its processes determine a nonuniformity and fleetingness in the properties of solar wind, the medium in which the planets exist. The velocity and concentration of interplanetary plasma and the size and direction of the interplanetary magnetic field may therefore vary substantially. The density of solar wind is very low and its magnetic field quite weak. How then do the planets react to such an ephemeral phenomenon? It turns out that the interaction of atmospheres, ionospheres and the magnetic fields of the individual planets with solar wind and the interplanetary magnetic field comprise a special area of planetary physics which is quite significant. The initial discoveries in this sphere were made, naturally, with respect to the Earth. The Earth as a strong magnetic field. It was established that solar wind meets this obstacle as it nears our planet and skirts around it. As a result, the solar wind seemingly draws lines of force of the Earth's magnetic field out away from the Sun, creating a so-called magnetospheric tail hundreds of thousands of kilometers in length and about 200,000 km in cross section.
Breus Tamara
Gringauz K.
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