Evidence for Compressive MHD Waves in the Solar Wind Near the Sun

Details Evidence for Compressive MHD Waves in the Solar Wind Near the Sun Evidence for Compressive MHD Waves in the Solar Wind Near the Sun

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh21a0721c&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH21A-0721

Physics

2149 Mhd Waves And Turbulence, 2169 Sources Of The Solar Wind, 7509 Corona

Scientific paper

Radio scattering observations in the inner solar wind provide a measure of the density fluctuations on scales of 2 to 50 km. Measurements with antenna arrays, such as the VLA and GMRT, show that this ``microscale turbulence'' is highly field-aligned, and the axial ratio of the structure decreases with increasing solar distance. In contrast, density fluctuations at scales between 1000 and 10,000 km appear to be almost isotropic. The microscale fluctuations also have a flatter spatial spectrum than the larger scale fluctuations (which have a Kolmogorov spectral exponent). Here we will present observations of multiple antenna intensity scintillation in the fast polar streams, which indicate that the speed of the microscale fluctuations is higher than the flow speed by approximately the Alfven speed. The observations, taken together, provide strong support for the suggestion (Harmon, 1989) that the microscale density fluctuations are caused by obliquely propagating Alfven waves. Detailed modeling shows that the observations are consistent with a mixture of Alfvén waves and slow magneto-acoustic waves, both of which must propagate obliquely outwards.

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