Computer Science – Sound
Scientific paper
Mar 1977
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1977sciam.236...36g&link_type=abstract
Scientific American, vol. 236, Mar. 1977, p. 36-43.
Computer Science
Sound
3
Flow Distribution, Magnetohydrodynamic Flow, Planetary Environments, Plasma Waves, Shock Wave Propagation, Solar Wind Velocity, Earth Atmosphere, Jupiter Atmosphere, Pioneer 10 Space Probe, Plasma Diagnostics, Rarefied Plasmas, Solar Atmosphere, Solar Corona, Solar Rotation, Wave Propagation
Scientific paper
The formation and evolution of velocity waves in the solar wind are discussed on the basis of spacecraft observations of the solar-wind stream structure. Variations in solar-wind speed are explained in terms of the expansion of different portions of the corona at different rates, the evolution of a velocity wave near earth is described, and the case of a single parcel of gas halfway up the leading edge of a solar-wind velocity wave is considered in detail. It is shown that a solar-wind wave will gradually be damped out if its peak speed is such that the speed of the gas converging on the parcel is less than the speed of sound and that a pair of shock waves will form if the speed of the converging gas exceeds the speed of sound. The predictions of a one-dimensional quantitative model of how solar-wind waves steepen are compared with observations by Pioneers 10 and 11 and IMP 7. The overall pattern of the solar wind in the plane of earth's orbit as it might appear to a stationary observer situated far above the north pole of the sun is deduced from the Pioneer 10 and IMP 7 data with the aid of a theoretical model. It is concluded that the concept of steepening velocity waves seems to explain the observed changes in solar-wind structure between 1 AU and about 5 AU and that the structure can be extended theoretically out to still more distant reaches of the solar system (beyond 20 AU, where the spiral pattern will begin to close back on itself).
Gosling Jack T.
Hundhausen Arthur J.
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