Finest Filamentary Structures of the Inner Corona in the Slow and Fast Solar Wind

Details Finest Filamentary Structures of the Inner Corona in the Slow and Fast Solar Wind Finest Filamentary Structures of the Inner Corona in the Slow and Fast Solar Wind

May 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996aas...188.8002w&link_type=abstract

American Astronomical Society, 188th AAS Meeting, #80.02; Bulletin of the American Astronomical Society, Vol. 28, p.956

Astronomy and Astrophysics

Astronomy

Scientific paper

Recent progress in the interpretation of angular scattering measurements has shown that a break in the vicinity of 1 Hz in the temporal frequency spectrum of electron density fluctuations provides a measure of the size of the finest filamentary structures in the solar corona. Using density spectra deduced from 1979-1980 Voyager joint phase scintillation and spectral broadening measurements by Coles et al. [1991], it is shown that the finest filamentary structures are found in the extensions or stalks of coronal streamers - the apparent sources of the slow solar wind - and are over a factor of three smaller than those in the fast wind emanating from coronal holes. The measured sizes of the finest filamentary structures are approximately 6 km in the slow wid at 8 Ro and 22 km in the fast wind at 9.1 Ro.

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