Spatial structure of solar wind at a time of minimum solar activity

Details Spatial structure of solar wind at a time of minimum solar activity Spatial structure of solar wind at a time of minimum solar activity

Mar 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983acasn..24..202z&link_type=abstract

(Acta Astronomica Sinica, vol. 24, 1983, p. 202-207) Chinese Astronomy and Astrophysics (ISSN 0275-1062), vol. 8, March 1984, p.

Astronomy and Astrophysics

Astrophysics

Interplanetary Medium, Interplanetary Space, Solar Activity Effects, Solar Corona, Solar Wind Velocity, Brightness Distribution, Current Sheets, Geomagnetic Latitude, Scintillation, Solar Cycles

Scientific paper

The 3D structure of the solar wind during the period of low solar activity in the first part of 1976 is investigated on the basis of K-corona (Hundhausen et al., 1981) and interplanetary-scintillation (Coles et al., 1980) observations. The average wind speed is shown to increase with increasing magnetic latitude (angular distance from the current sheet) out to + or - 35 deg, beyond which it remains constant at about 600 km/sec. Since the maximum brightness curve moves away from the solar equator at frequent intervals during the period, the wind-speed distribution is asymmetrical about the equator and depends on the global polarity distribution of the interplanetary magnetic field.

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