Magnetic Helicity Transport in the Quiet Sun: Theory & Observations

Details Magnetic Helicity Transport in the Quiet Sun: Theory & Observations Magnetic Helicity Transport in the Quiet Sun: Theory & Observations

Dec 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001agufmsh11c0721w&link_type=abstract

American Geophysical Union, Fall Meeting 2001, abstract #SH11C-0721

Physics

7524 Magnetic Fields, 7529 Photosphere, 7544 Stellar Interiors And Dynamo Theory

Scientific paper

The flux of magnetic helicity through the solar photosphere has implications in diverse areas of current solar research, including solar dynamo and solar wind modeling. Various authors have considered the flux of magnetic helicity from active regions (e.g., DeVore, 2000; Chae, 2001); here, we do the same for magnetic fields in the quiet sun. We express the helicity flux in terms of the relative motions and deformations of isolated magnetic flux elements, summing both ``mutual helicity" and ``self-helicity" contributions to get the total helicity flux. Using a tracking algorithm applied to high cadence, high resolution SOHO/MDI magnetograms, we determine the observed rate of helicity flux in the quiet sun and compare these measurements with our theoretical predictions.

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