The Small-Scale Field Measured With Hinode/SOT and Feature Tracking: Where is the mixed- polarity flux?

Details The Small-Scale Field Measured With Hinode/SOT and Feature Tracking: Where is the mixed- polarity flux? The Small-Scale Field Measured With Hinode/SOT and Feature Tracking: Where is the mixed- polarity flux?

May 2008

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008agusmsp51d..01d&link_type=abstract

American Geophysical Union, Spring Meeting 2008, abstract #SP51D-01

Physics

7524 Magnetic Fields, 7526 Magnetic Reconnection (2723, 7835), 7529 Photosphere, 7544 Stellar Interiors And Dynamo Theory, 7594 Instruments And Techniques

Scientific paper

We report on the results of the first feature tracking study of the solar magnetic field with Hinode/SOT. We processed a SOT Na-D line-of-sight magnetogram sequence with five different magnetic tracking codes. The SOT data allow us to probe the evolving magnetic field on the granular scale for hours at a time, something that was not possible with either ground-based observations (which are limited to short periods of good seeing) or prior space-based observations (which are limited to arcsecond spatial scales). We find that the field is much less mixed than previously supposed: while Hinode resolves small-scale structure within features that, to SOHO/MDI, would appear as monolithic flux concentrations, this substructure has but a single sign. Furthermore, the average distance between identifiable flux concentrations of opposite sign remains nearly unchanged at the higher resolution, a result that is quite surprising in light of the common picture of a sea of strong mixed-polarity flux concentrations dotting the inter-granular lanes. We discuss possible mechanisms for this surprising result, and implications for the small-scale dynamo.

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