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Article overview
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Photospheric Electric Fields and Energy Fluxes in the Eruptive Active Region NOAA 11158 | | Maria D. Kazachenko
; George H. Fisher
; Brian T. Welsch
; Yang Liu
; Xudong Sun
; | | Date: |
22 May 2015 | | Abstract: | 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 NOAA active region 11158, which produced an X2.2
flare early on 2011 February 15. We find photospheric electric fields ranging
up to $1.5$ V/cm. The Poynting fluxes range up to $2 imes10^{10}$
ergs$cdot$cm$^{-2}$s$^{-1}$ with mean values around $10^8$-$10^9$
ergs$cdot$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 emergence to the moment before the X2.2 flare to be
$E=10.6 imes10^{32}$ ergs, which is partitioned as $2.0 imes10^{32}$ ergs and
$8.6 imes10^{32}$ ergs, respectively, between free and potential energies.
Those estimates are consistent with estimates from pre-flare 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. | | Source: | arXiv, 1505.5974 | | Services: | Forum | Review | PDF | Favorites | |
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