Direct observation of the latitudinal extent of a high-speed stream in the solar wind

Details Direct observation of the latitudinal extent of a high-speed stream in the solar wind Direct observation of the latitudinal extent of a high-speed stream in the solar wind

Mar 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978jgr....83.1011s&link_type=abstract

Journal of Geophysical Research, vol. 83, Mar. 1, 1978, p. 1011-1017. Research supported by the Deutsche Bundesministerium für

Physics

32

Satellite Observation, Solar Corona, Solar Wind Velocity, Helios 1, Imp, Interplanetary Medium, Solar Corpuscular Radiation, Spatial Distribution

Scientific paper

The latitudinal boundaries of stationary fast solar wind streams emerging from equatorward extensions of the sun's polar coronal holes are studied. Simultaneous data from the Helios 1 and Imp spacecraft at different heliographic latitudes are compared. The measured latitudinal speed gradient of 30 km/s/deg shows that large angular speed gradients occur at the leading edges of fast streams and also with respect to latitude. The data indicate that longitudinal speed gradients are steeper near 0.3 AU than at 1.0 AU. Generally, regions with large angular speed gradients are observed to separate fast streams from the surrounding slower plasma. This suggests the existence of mechanisms which diminish longitudinal speed gradients as the plasma travels toward 1.0 AU. It also seems that the distribution of solar wind speeds on a near-sun spherical surface has large mesalike high-speed regions. Comparisons of Helios 1 and Imp data with corona observations supports the hypothesis that high-speed solar wind streams emerge from coronal holes.

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