We plan a study of magnetic flux dispersal in the solar photosphere. Properties and mechanisms of the flux dispersal can be used as important constrains and clues for dynamo theories. Large-scale dynamo models essentially depend on the flux transport models, which require the magnitude of diffusivity of about 600 km^2/s on supergranular scales, which is 2-3 times higher than observed diffusivity. Local turbulent dynamo, to be successful in generation of small-scale flux tubes, requires very small magnitudes of diffusivity on small scales. Observational and model data for the entire spectrum of diffusivity on all scales are definitely required now to make a further step in understanding of the solar magnetism.
A combination of New Solar Telescope (NST) and Hinode SOT magnetograms and filtergrams will enable significant progress in understanding magnetic flux dispersal over the solar surface.
We will use this data to detect and track magnetic elements (Hinode/FG magnetograms) and bright points (NST/TiO, G-band, Hinode G-band).
We will extend this study on all types of magnetic configuration and we want to start with coronal holes, where the numbers of bright points is not high, so the analysis may be a bit simplier. |
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