Three-dimensional structure of the solar wind: Variation of density with the solar cycle

Details Three-dimensional structure of the solar wind: Variation of density with the solar cycle Three-dimensional structure of the solar wind: Variation of density with the solar cycle

Nov 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993soph..148..153m&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 148, no. 1, p. 153-167

Astronomy and Astrophysics

Astronomy

46

Electron Density (Concentration), Flux Density, Plasma Density, Plasma Turbulence, Radio Astronomy, Radio Sources (Astronomy), Scintillation, Solar Cycles, Solar Wind, Density Distribution, Heliosphere, Radio Telescopes, Sunspots

Scientific paper

Interplanetary Scintillation (IPS) measurements obtained from a large number of compact radio sources (nearly 150 sources) distributed over the heliocentric distance range 15-175 solar radii and heliographic latitude approximately 75 deg N-75 deg S have been used to study the global three-dimensional density distribution of the solar wind plasma. Contours of constant electron-density fluctuations (Delta Ne) in the heliospheric plasma obtained for both the solar minimum and maximum show a strong solar latitude dependence. During low solar activity, the equatorial density-fluctuation value decreases away from the equator towards higher latitudes and is reduced by approximately 2.5 times at the poles; the level of turbulence is reduced by a factor of approximately 7; the solar-wind mass flux density at the poles is approximately 25% lower than the equatorial value. However, during high solar activity, the average distribution of density fluctuations becomes spherically symmetric. In the ecliptic, the variation of Delta Ne with the heliocentric distance follows a power law of the form R-2.2 and it does not show any change with solar activity.

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