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Estimates of the photospheric magnetic, electric and plasma velocity fieldsare essential for studying the dynamics of the solar atmosphere, for examplethrough the derivative quantities of Poynting and relative helicity flux and byusing of the fields to obtain the lower boundary condition for data-drivencoronal simulations. In this paper we study the performance of a dataprocessing and electric field inversion approach that requires onlyhigh-resolution and high-cadence line-of-sight or vector magnetograms -- whichwe obtain from Helioseismic and Magnetic Imager (HMI) onboard Solar DynamicsObservatory (SDO). The approach does not require any photospheric velocityestimates, and the lacking velocity information is compensated using ad hocassumptions. We show that the free parameters of these assumptions can beoptimized to reproduce the time evolution of the total magnetic energyinjection through the photosphere in NOAA AR 11158, when compared to the recentestimates for this active region. However, we find that the relative magnetichelicity injection is reproduced poorly reaching at best a modestunderestimation. We discuss also the effect of some of the data processingdetails on the results, including the masking of the noise-dominated pixels andthe tracking method of the active region, both of which have not received muchattention in the literature so far. In most cases the effect of these detailsis small, but when the optimization of the free parameters of the ad hocassumptions is considered a consistent use of the noise mask is required. Theresults found in this paper imply that the data processing and electric fieldinversion approach that uses only the photospheric magnetic field informationoffers a flexible and straightforward way to obtain photospheric magnetic andelectric field estimates suitable for practical applications such as coronalmodeling studies.

Optimization of Photospheric Electric Field Estimates for Accurate Retrieval of Total Magnetic Energy Injection