Magnetic Flux Cancellation and Coronal Magnetic Energy

Details Magnetic Flux Cancellation and Coronal Magnetic Energy Magnetic Flux Cancellation and Coronal Magnetic Energy

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusmsh53b..06w&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #SH53B-06

Physics

7507 Chromosphere, 7513 Coronal Mass Ejections, 7524 Magnetic Fields, 7529 Photosphere, 7531 Prominence Eruptions

Scientific paper

I investigate the processes at work in the cancellation of normal magnetic flux in solar magnetograms, and study the relationships between cancellation and the budget of free energy in the coronal magnetic field that can power solar flares and CMEs. I begin by defining cancellation, and, focusing on reconnective cancellation, present the relevant equations describing the field evolution during cancellation. I then analyze these equations, to show that: 1) cancellation tends to reduce the magnetic energy of the hypothetical "open" field state; 2) in a sheared arcade field, steady cancellation adds free energy to the actual coronal field; and 3) horizontal magnetic flux can diffuse at a rate much lower than does the cancelling normal flux, even in the presence of constant resistivity. Finally, I briefly discuss the implications of boundary conditions in numerical simulations of flux cancellation.

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