ForumSpringer[A&A-EE Home Page]
ForumWhats NewSearchOrdersTable of Contents

Astron. Astrophys. 316, 449-456 (1996)

Coronal radio sounding with Ulysses: dual-frequency phase scintillation spectra in coronal holes and streamers

M. Pätzold1, J. Karl1, and M.K. Bird2

1 Institut für Geophysik und Meteorologie, Universität zu Köln, Albertus-Magnus-Platz, D-50923 Köln, Germany
2 Radioastronomisches Institut, Universität Bonn, Auf dem Hügel 71, D-53121 Bonn, Germany

Received 18 March 1996 / Accepted 20 August 1996

Abstract. Dual-frequency Doppler measurements of the Ulysses downlink carrier signals were recorded during the spacecraft's 1995 solar conjunction. In this paper we present power spectra derived from phase fluctuations of the radio signals passing through the corona for different solar latitudes. It is possible to (a) distinguish clearly between spectra for which the ray paths were entirely embedded in a coronal hole or traversed a coronal streamer for the same solar offset distance of 25 solar radii and (b) characterize the evolution of the slope of the phase fluctuation spectra p-1 as a function of heliolatitude, where p is the spectral index of the three-dimensional wavenumber spectrum of the electron density fluctuations. There is an obvious increase from p=3.2 at high southern latitudes (coronal hole) toward the Kolmogorov value of p=11/3 at those heliolatitudes coinciding with the extension of the heliospheric current sheet. The spectra show a local flattening with break frequencies at 0.06 Hz and 0.2 Hz for the hole and the streamer spectra, respectively. The shift from 0.06 Hz to 0.2 Hz is not gradual, but rather abrupt when the ray path becomes embedded in the streamer. The derived electron density fluctuations and fractional electron density fluctuations at 25 solar radii are larger in the coronal streamer than in the coronal hole by factors of img1.gif 20 and img1.gif 5, respectively.

Key words: Sun: corona - solar wind - occultation

Article in PDF format
Article in (gzipped) PS format

Last change: December 30, 1996
© European Southern Observatory (ESO) 1996