Effect of coronal magnetic fields on the formation of the solar wind from radio polarization occultation data

Details Effect of coronal magnetic fields on the formation of the solar wind from radio polarization occultation data Effect of coronal magnetic fields on the formation of the solar wind from radio polarization occultation data

Apr 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999arep...43..267e&link_type=abstract

Astronomy Reports, Volume 43, Issue 4, April 1999, pp.267-274

Astronomy and Astrophysics

Astronomy

Scientific paper

An analysis of radio occultation of the near-solar plasma using linearly polarized S-band (2.3 GHz) signals from the HELIOS-1 and HELIOS-2 spacecraft is presented. Fluctuations in the Faraday rotation of the plane of polarization were measured simultaneously at three widely spaced ground stations of the NASA Deep Space Network at Canberra, Madrid, and Goldstone. The temporal energy spectra of the Faraday-rotation fluctuations (FRF) were obtained using measurements in 1981 and 1983 for heliocentric distances R = (3_12)R_S (R_S is the solar radius). We have studied the dependences of the shape and variance of the FRF spectra on heliocentric distance. The power-law index for the two-dimensional FRF spatial spectrum is close to beta = 2 for heliocentric distances R = (3_6)R_S, and decreases with distance from the Sun, reaching the value beta = 1.2 at R = 10R_S. Comparison with earlier measurements of the power-law index beta' for radio-occultation phase-fluctuation spectra shows that beta ~= beta' when R = (3_6)R_S and beta < beta' ~= 2 at larger distances. The time lag between the FRF for different receiving stations was measured using a cross-correlation analysis, enabling determination of the velocities of the irregularities, which are in good agreement with the expected Alfven speed. The correlation between temporal variations of the fluctuation intensity and the time lag is studied. The FRFs are primarily determined by Alfven waves. The solar wind regime in the acceleration region is governed by coronal magnetic fields.

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