Radio interferometer observations of turbulence in the inner solar wind

Details Radio interferometer observations of turbulence in the inner solar wind Radio interferometer observations of turbulence in the inner solar wind

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aipc..382..265s&link_type=abstract

Proceedings of the eigth international solar wind conference: Solar wind eight. AIP Conference Proceedings, Volume 382, pp. 265

Computer Science

2

Solar Wind Plasma, Sources Of Solar Wind, Plasma Turbulence

Scientific paper

Measurements can be made of Very Long Baseline Interferometer (VLBI) phase scintillations due to plasma turbulence in the solar corona and solar wind. These measurements provide information on the spectrum and intensity of density fluctuations with scale sizes of a few hundred to several thousand kilometers. If we model the spatial power spectrum of the density fluctuations as Pδn(q)=CN2q-α, where q is the spatial wavenumber, these observations yield both α and the path-integrated value of CN2. The recently completed Very Long Baseline Array (VLBA) is capable of making such measurements over the heliocentric distance range from a few solar radii to 60 solar radii and beyond. This permits the determination, with the same technique and instrument, of the radial evolution of turbulent characteristics, as well as their dependence on solar wind transients, sector structure, etc. In this paper we present measurements of 16 sources observed at a wide range of solar elongations and at different times. These observations show that the coefficient CN2 depends on heliocentric distance as approximately CN2~(R/Rsolar)-3.7. The radio derived power spectral characteristics are in agreement with in situ measurements by the Helios spacecraft for regions of slow solar wind, but fast solar wind does not have large enough density fluctuations to account for the magnitude of the observed scintillations. The observed radial dependence is consistent with a Wentzel-Kramers-Brillouin (WKB)-type evolution of the turbulence with heliocentric distance.

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