Steven R. Spangler University of Iowa

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Presentation transcript:

Steven R. Spangler University of Iowa Observations of Density Fluctuations Near the Sun Using Radio Scintillations Steven R. Spangler University of Iowa

Basic physics of extracting information on coronal turbulence: radio refractive index Radio propagation effects primarily diagnose density fluctuations Are secondary indicators of B

Example: Phase Scintillations of a VLBI Interferometer

Types of Scintillation Phenomena Frequency scintillation Intensity cross-correlation

Principal Papers In This Area Deduction of plasma physical properties from radio observations Harmon & Coles 2005, JGR 110, 031001H Hollweg et al 1982, JGR 87, 1

Radio Results on Coronal Turbulence I: Speed of irregularities << VA : Irregularities are non-propagating or oblique AIC waves

Radio Results on Coronal Turbulence II: Density spectrum power law with “bulge” at ion inertial length (Coles and Harmon, 1989ff)

Radio Results on Coronal Turbulence III: Smooth variation of turbulent intensity with heliocentric distance; no coronal “Kumasphere”. Not unanimous; see Lotova

Open Questions and Issues for Discussion Why no fast mode waves in corona? (Harmon and Coles). Similar situation in ISM. What are the amplitudes of velocity and magnetic fluctuations? Is the turbulence sufficiently strong to heat and accelerate? How is the turbulence generated? Thanks