Photospheric Electric Fields and Energy Fluxes in the Eruptive Active Region NOAA 11158
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Introduction
The advent of high-cadence vector magnetic field and Doppler velocity measurements from e.g. HMI/SDO, SOT/Hinode and SOLIS, have made the estimation of electric fields in the solar photosphere possible. The calculation of the electric field from magnetic and Doppler data is critically important for various quantitative studies of the solar atmosphere. First, if we know both electric and magnetic field vectors in the photosphere, we can estimate both the Poynting flux of magnetic energy and the flux of relative magnetic helicity entering the corona. Second, knowledge of electric and magnetic fields enables the driving of time-dependent simulations of the coronal magnetic field. This is the goal of the Coronal Global Evolutionary Model (CGEM, Fisher et al. 2015).
Method
We have recently improved the electric field inversion methods introduced by Fisher et al. (2010), to create a comprehensive technique for calculating photospheric electric fields from vector magnetogram sequences (Kazachenko et al. 2014). The new method, which we dubbed the PDFI (an abbreviation for PTD-Doppler-FLCT-Ideal technique, where PTD and FLCT stand for Poloidal-Toroidal Decomposition and Fourier Local Correlation Tracking), has been systematically tested for accuracy and robustness, using synthetic data from ANMHD simulations. Here we take the next step forward, and apply the PDFI technique to observations.
Dataset
The flare-productive active region (AR) NOAA 11158 was observed by HMI nearly continuously for a six-day period over 2011 February 10–16 from its emergence (see Bz-snapshots in Figure 1). We used the sequence of 770 vector magnetic field B and Doppler field measurements to derive the temporal evolution of electric fields E and Poynting S fluxes during these six days.
Results
To describe the photospheric electric fields E and energy fluxes S in NOAA 11158, we use two approaches: we first show the spatial distribution of B, E and S at two times, before and after the X2.2 flare; we then analyze their temporal spatially integrated evolution over six days of observations.
Magnetic Field: Bpreflare and Bpostflare
Pre- and post-flare snapshots of the vertical magnetic field (Figure 2) show that the horizontal magnetic field close to PIL increased by over 300 G during the X2.2 flare (see arrows), while the vertical magnetic field remained nearly constant, consistent with the field implosion scenario. On the difference image (right panel) we also notice two circular patterns, directed counter-clockwise in negative and clockwise in positive polarities, implying that the field connecting those polarities becomes less twisted.
Electric Field: Epreflare and Epostflare
We find the photospheric electric field vector, ranging from -2 to 2 V/cm, to increase its magnitude by up to 0.5 V/cm at the PIL and 1 V/cm away from the PIL during the flare (Figure 3). The horizontal component is mostly concentrated along the PIL, while the vertical component is largest at the PIL and in the sunspots’ penumbrae. The presence of a nonzero Ez is related to changes in the vertical current, which is mostly concentrated close to the main PIL (Petrie 2013; Janvier et al. 2014).