Astronomy and Astrophysics – Astronomy
Scientific paper
May 1975
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975jgr....80.1845h&link_type=abstract
Journal of Geophysical Research, vol. 80, May 1, 1975, p. 1845-1848.
Astronomy and Astrophysics
Astronomy
7
Astronomical Models, Fluid Boundaries, Periodic Variations, Solar Wind, Gas Dynamics, Magnetohydrodynamic Flow, Plasma Density, Plasma Temperature, Solar Wind Velocity
Scientific paper
The basic variations in solar wind properties that have been observed at 'stream interfaces' near 1 AU are explained by a gas dynamic model in which a radially propagating stream, produced by a temperature variation in the solar envelope, steepens nonlinearly while moving through interplanetary space. The region thus identified with the stream interface separates the ambient solar wind from the fresh hot material originally in the stream. However, the interface regions given by the present model are thicker than most stream interfaces observed in the solar wind, a fact suggesting that some additional physical process may be important in determining that thickness. Variations in the density, speed, or Alfven pressure alone appear not to produce streams with such an interface.
Burlaga Leonard Francis
Hundhausen Arthur J.
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