EDP Sciences
Free access
Volume 384, Number 2, March III 2002
Page(s) 654 - 665
Section The Sun
DOI http://dx.doi.org/10.1051/0004-6361:20020028

A&A 384, 654-665 (2002)
DOI: 10.1051/0004-6361:20020028

Very Long Baseline Interferometer measurements of turbulence in the inner solar wind

S. R. Spangler1, 2, D. W. Kavars1, P. S. Kortenkamp1, M. Bondi2, F. Mantovani2 and W. Alef3

1  Dept. of Physics and Astronomy, University of Iowa, Iowa City, Iowa 52242, USA
2  Istituto di Radioastronomia del CNR, Via Gobetti 101, 40129 Bologna, Italy
3  Max-Planck-Institut für Radioastronomie, Auf dem Hügel 69, 53121 Bonn, Germany

(Received 3 July 2001 / Accepted 4 January 2002 )

Very Long Baseline Interferometry (VLBI) observations were made of six sources in September and 1998. The observations were made at a time when the solar elongations of five of those sources ranged from $4\fdg 4$ to $6\fdg8$, so that the lines of sight to these sources passed at distances of closest approach to the Sun of 16.5 to 25.3  $R_{\odot}$. The solar elongation of the sixth source was $16\fdg6$, corresponding to a distance of $62.4~R_{\odot}$. The observations were made with the Medicina and Noto antennas of the Istituto di Radioastronomia, the Matera (Italy) antenna of the Agenzia Spaziale Italiana, and the Wettzell (Germany) antenna of the Bundesamt für Kartographie und Geodäsie. On two of the three days of observation (September 24 and October 15, 1998) simultaneous observations were made at 8.380 ( X band) and 2.257 ( S band) GHz. In the third observing session (September 25, 1998) observations were made at 4.981 GHz ( C band). Temporal fluctuations in the interferometer phase, induced by the solar wind, were analysed to yield information on plasma turbulence in the inner heliosphere. The results of this investigation are as follows. (1) The measured interferometer phase power spectra are consistent with a theoretical expression which incorporates independent information on solar wind turbulence. (2) The values for  $C_{\rm N}^2$, the normalization constant of the density power spectrum, are reasonably consistent with a previously-determined expression for $C_{\rm N}^2(r)$, where r is the heliocentric distance, although the new values for $C_{\rm N}^2$ are systematically high with respect to this prior expression. (3) Our estimates for the speed at which the irregularities move with respect to the antennas, and in the radial direction from the Sun, are in the range of 190-340 km s -1 for heliocentric distances of 16-26  $R_{\odot}$. These values are in good agreement with observational estimates of the solar wind flow speed in this part of space based on coronagraph observations. The speeds are lower than the sum of the estimated solar wind flow speed and the local Alfvén speed. The potential significance of this result is discussed.

Key words: solar wind -- Sun: corona -- turbulence

Offprint request: S. Spangler, srs@astro.physics.uiowe.edu

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