Interplanetary scintillation and the structure of the solar wind transonic region

Details Interplanetary scintillation and the structure of the solar wind transonic region Interplanetary scintillation and the structure of the solar wind transonic region

Sep 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985a%26a...150..266l&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 150, no. 2, Sept. 1985, p. 266-272.

Astronomy and Astrophysics

Astrophysics

49

Interplanetary Medium, Scintillation, Solar Wind, Transonic Flow, Radial Distribution, Subsonic Flow, Water Masers

Scientific paper

The results of scintillation studies of the interplanetary medium close to the sun are given. The use of water vapor maser sources enables investigations in the weak scattering regime in both the transonic and the subsonic regions of the solar wind. The radial dependence of the scintillation index m in the subsonic region, at solar elongations ranging from 4 solar radii to about 10 solar radii is found to be m varying as R to the -1.6 + or -0.1. The existence of a previously unknown enhanced scintillation region stretching from about 10 to 20 solar radii is reported. Considering the large-scale velocity field irregularities of the solar wind stream structure, the transonic region may be treated as a region of mixed flow, where subsonic and supersonic streams coexist and interact. It is shown that the stream structure of the solar wind is one of the principal factors in the formation of the extended (about 10 solar radii) transonic region. The localization and other parameters of the transonic region display pronounced changes in response to variations in solar activity.

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