Scaling Properties of Solar Magnetic and Velocity Fields

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The PI will study the scaling symmetry of spatial and temporal structure of solar magnetic and velocity fields to trace their physical origins in the convective solar plasma. First, she will investigate the range of physical scales and magnetic filed strengths over which multifractal symmetry applies on the Sun. Wavelet transforms will localize image sites where the magnetic field strength appears to show singular behavior. The PI will observe the relation between these sites and unresolved magnetic structures, such as flux-tubes. She will then distinguish between zero or transverse field configurations versus rapidly reversing fields using the scaling symmetry of fluctuations in the direction of the magnetic vector field. By examining Doppler images, the PI will determine the form of scaling and, thus, of the transport in the photosphere. Finally, the PI will examine a diverse array of effective models for the generation of observed magnetic field structuring and scaling symmetry.