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

¹ Jodrell Bank Centre for Astrophysics, University of Manchester, Manchester M13 9PL, UK
e-mail: mykola.gordovskyy@manchester.ac.uk
² Faculty of Science, Engineering and Built Environment, Deakin University, Melbourne, VIC 3125, Australia
³ Astronomical Observatory of the Taras Shevchenko National University of Kyiv, Observatorna 3, Kyiv 04053, Ukraine

Received: 30 October 2019
Accepted: 3 December 2019

Abstract

Aims. The goal of this study is to explore a novel method for the solar photospheric magnetic field diagnostics using Stokes V widths of different magnetosensitive Fe I spectral lines.

Methods. We calculate Stokes I and V profiles of several Fe I lines based on a one-dimensional photospheric model VAL C using the NICOLE radiative transfer code. These profiles are used to produce calibration curves linking the intrinsic magnetic field values with the widths of blue peaks of Stokes V profiles. The obtained calibration curves are then tested using the Stokes profiles calculated for more realistic photospheric models based on magnetohydrodynamic of magneto-convection.

Results. It is shown that the developed Stokes V widths method can be used with various optical and near-infrared lines. Out of six lines considered in this study, Fe I 6301 line appears to be the most effective: it is sensitive to fields over ∼200 G and does not show any saturation up to ∼2 kG. Other lines considered can also be used for the photospheric field diagnostics with this method, however, only in narrower field value ranges, typically from about 100 G to 700–1000 G.

Conclusions. The developed method can be a useful alternative to the classical magnetic line ratio method, particularly when the choice of lines is limited.