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Photospheric Electric Fields and Energy Fluxes in the Eruptive Active Region NOAA 11158 View all abstracts by submitter

Maria D Kazachenko   Submitted: 2015-08-17 12:26

How much electromagnetic energy crosses the photosphere in evolving solar active regions? With the advent of high-cadence vector magnetic field observations, addressing this fundamental question has become tractable. In this paper, we apply the "PTD-Doppler-FLCT-Ideal" (PDFI) electric field inversion technique of Kazachenko et al. (2014) to a 6-day HMI/SDO vector magnetogram and Doppler velocity sequence, to find the electric field and Poynting flux evolution in active region NOAA 11158, which produced an X2.2 flare early on 2011 February 15. We find photospheric electric fields ranging up to 2 V/cm. The Poynting fluxes range from [-0.6 to 2.3]*1010 ergs cm-2 s-1, mostly positive, with the largest contribution to the energy budget in the range of [109-1010] ergs cm-2 s-1. Integrating the instantaneous energy flux over space and time, we find that the total magnetic energy accumulated above the photosphere from the initial emergence to the moment before the X2.2 flare to be E=10.6*1032 ergs, which is partitioned as 2.0 and 8.6*1032 ergs, respectively, between free and potential energies. Those estimates are consistent with estimates from preflare non-linear force-free field (NLFFF) extrapolations and the Minimum Current Corona estimates (MCC), in spite of our very different approach. This study of photospheric electric fields demonstrates the potential of the PDFI approach for estimating Poynting fluxes and opens the door to more quantitative studies of the solar photosphere and more realistic data-driven simulations of coronal magnetic field evolution.

Authors: Kazachenko, Maria D.; Fisher, George H.; Welsch, Brian T.; Liu, Yang; Sun, Xudong
Projects: SDO-HMI

Publication Status: 51 pages, 10 figures, accepted by ApJ on August 11, 2015
Last Modified: 2015-08-17 15:10
Go to main E-Print page  Chromospheric Evaporation in an X1.0 Flare on 2014 March 29 Observed with IRIS and EIS  Comparison between the eruptive X2.2 flare on 2011 February 15 and confined X3.1 flare on 2014 October 24  Edit Entry  Download Preprint  Delete Entry 

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