The investigation of the solar wind transonic region at meter wavelengths

Details The investigation of the solar wind transonic region at meter wavelengths The investigation of the solar wind transonic region at meter wavelengths

Sep 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988soph..117..407l&link_type=abstract

(Solar Cycle Workshop, Meeting, 2nd, Lake Tahoe, CA, May 1987) Solar Physics (ISSN 0038-0938), vol. 117, no. 2, 1988, p. 407-414

Astronomy and Astrophysics

Astronomy

6

Interplanetary Medium, Radio Astronomy, Solar Wind Velocity, Space Plasmas, Quasars, Subsonic Flow, Supersonic Flow, Transonic Flow, Water Masers

Scientific paper

Radio astronomy experiments designed to probe the interplanetary plasma close to the sun have been carried out at the wavelength lambda = 2.92 m using the occultation method. The experiments are based on a modification of the occultation method by which the sources, in this case quasars, are used to measure the radial dependence of the apparent source size, the scattering angle theta(R). The radial dependence of this source size theta(R) reveals that an anomalous enhancement in the scattering appears at radial distances from about 16 to 30 solar radii, which is associated with the solar wind transsonic region. It is shown by analysis of the theoretical equations that the radial profiles of both the source size theta(R) and the scintillation index m(R) are consistent in the near solar interplanetary medium. Combining these two independent applications of the occultation method extends the range of the investigation and provides a powerful new diagnostic of the solar wind transsonic region.

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