Measurements of Free Magnetic Energy Flux Across the Photosphere

Details Measurements of Free Magnetic Energy Flux Across the Photosphere Measurements of Free Magnetic Energy Flux Across the Photosphere

Dec 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agufmsh13a0270w&link_type=abstract

American Geophysical Union, Fall Meeting 2005, abstract #SH13A-0270

Physics

7513 Coronal Mass Ejections (2101), 7519 Flares, 7524 Magnetic Fields, 7529 Photosphere, 7594 Instruments And Techniques

Scientific paper

Solar flares and CMEs are thought to be powered by free energy in the coronal magnetic field. Several theoretical models make testable predictions about how this free magnetic energy enters the corona through the photosphere (e.g., cancellation, or shear along polarity inversion lines). Further, some observers have suggested particular mechanisms (e.g., rotating sunspots) might play an important role in transporting free magnetic energy into the corona. In addition, the flux of free energy might be correlated with local coronal heating, which could lead to EUV and/or X-ray emission. Here, we present formalism that allows determination of the flux density of free magnetic energy from a time series of vector magnetograms and results derived from velocity inversion techniques (e.g., local correlation tracking, or inductive local correlation tracking). We then apply this approach to time series of vector magnetograms, and compare: 1) the locations of measured free energy flux with the predictions of both modelers and observers; 2) our integrated free energy flux with typical flare and CME energies; and 3) Yohkoh SXT images of the corona above these active regions.

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