The latitude and longitude structure of the solar wind speed from IPS observations

Details The latitude and longitude structure of the solar wind speed from IPS observations The latitude and longitude structure of the solar wind speed from IPS observations

Dec 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978jgr....83.5757s&link_type=abstract

Journal of Geophysical Research, vol. 83, Dec. 1, 1978, p. 5757-5762.

Astronomy and Astrophysics

Astronomy

11

Coronal Holes, Interplanetary Space, Radio Observation, Scintillation, Solar Corona, Solar Wind Velocity, Latitude Measurement, Longitude Measurement, Radial Velocity, Radio Sources (Astronomy), Signal Measurement, Spatial Distribution, Velocity Distribution

Scientific paper

Interplanetary scintillation (IPS) observations are used to develop a picture of the distribution of solar-wind velocities in latitude and longitude. Such a picture is derived for periods of several rotations during the years 1973-1977. The observations are interpreted as if they were point observations and mapped to the sun with the constant radial velocity assumption. Since only eight scintillating radio sources are available, a useful instantaneous picture cannot be obtained, so some integration in time is required to build up coverage. The observed average velocity distributions are found not to be isotropic or even symmetric about the rotation axis of the sun. The averaged distributions are found to be similar to and to evolve as the distribution of low intensities in white-light coronameter data taken at 1.5 solar radii and suggest that high-speed solar wind originates in regions of low coronal density. This extends to high latitudes the evidence for coronal holes as the source of high-speed streams, including polar holes as the source of high speeds at polar latitudes.

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