Temporal Evolution of Free Magnetic Energy Associated with Four X-Class Flares

Details Temporal Evolution of Free Magnetic Energy Associated with Four X-Class Flares Temporal Evolution of Free Magnetic Energy Associated with Four X-Class Flares

May 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009apj...696...84j&link_type=abstract

The Astrophysical Journal, Volume 696, Issue 1, pp. 84-90 (2009).

Astronomy and Astrophysics

Astronomy

13

Sun: Activity, Sun: Corona, Sun: Flares, Sun: Magnetic Fields

Scientific paper

We study the temporal variation of free magnetic energy E free around the time of four X-class flares. The high-cadence photospheric vector magnetograms obtained by the digital vector magnegograph system at the Big Bear Solar Observatory are used as the boundary conditions to reconstruct the three-dimensional nonlinear force-free (NLFF) coronal field. In order to remove the effect of the net Lorentz force and torque acting in the photosphere, the vector magnetograms are preprocessed using the method devised by Wiegelmann et al.. Then a well-tested multigrid-like optimization code by Wiegelmann is applied to the preprocessed boundary data to extrapolate the NLFF coronal field with which we are able to estimate the free energy E free. In all the four events, we find a significant drop of E free starting ~15 minutes before the peak time of the associated nonthermal flare emission, although long-term trend varies from event to event. We discuss the physical implication of the result, i.e., the magnetic relaxation is already going on in the corona well before the flare reconnection.

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