Inference of electric currents in the solar photosphere

We aim at demonstrating the capabilities of a newly developed method for determining electric currents in solar photosphere. employ three-dimensional radiative magneto-hydrodynamic (MHD) simulations to produce synthetic Stokes profiles several spectral lines with spatial resolution similar what operational 4-meter Daniel K. Inouye Solar Telescope (DKIST) telescope should achieve. apply inversion polarized transfer equation magneto-hydrostatic (MHS) constraints infer magnetic field vector Cartesian domain, $\mathbf{B}(x,y,z),$ from profiles. then Ampere's law determine currents, ${\bf j}$, inferred field, and compare results present original MHD simulation. show that employed here is able attain reasonable reliability (close 50 % cases are within factor two, this increases 60 %-70 pixels $B\ge300$ G) inference low atmospheric heights (optical depths 500 nm $\tau_{5}\in$[1,0.1]) regardless whether small or large number inverted. Above these photospheric layers, method's accuracy strongly deteriorates as fields become weaker MHS approximation becomes less accurate. also find have floor value related low-magnetized plasma, where uncertainty prevents sufficiently accurate determination derivatives. allows three components current deep layers (photospheric layers) spectropolarimetric observations.