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The goal of this study is to explore a novel method for the solarphotospheric magnetic field diagnostics using Stokes V widths of differentmagnetosensitive Fe~I spectral lines. We calculate Stokes I and V profiles ofseveral Fe I lines based on a one-dimensional photospheric model VAL C usingthe NICOLE radiative transfer code. These profiles are used to producecalibration curves linking the intrinsic magnetic field values with the widthsof blue peaks of Stokes V profiles. The obtained calibration curves are thentested using the Stokes profiles calculated for more realistic photosphericmodels based on MHD models of magneto-convection. It is shown that thedeveloped Stokes V widths (SVW) method can be used with various optical andnear-infrared lines. Out of six lines considered in this study, FeI 6301 lineappears to be the most effective: it is sensitive to fields over ~200G and doesnot show any saturation up to ~2kG. Other lines considered can also be used forthe photospheric field diagnostics with this method, however, only in narrowerfield value ranges, typically from about 100G to 700-1000G. The developedmethod can be a useful alternative to the classical magnetic line ratio method,particularly when the choice of lines is limited.

Using the Stokes V widths of Fe I lines for diagnostics of the intrinsic solar photospheric magnetic field