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 magnetiosensitive 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 radiative transfer code NICOLE. 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 MHD models of magneto-convection.
Results. It is shown that the developed Stokes V widths (SVW) 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 considered lines can also be used for the photospheric field diagnostics with this method, however, 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.
Methods. We calculate Stokes I and V profiles of several Fe I lines based on a one-dimensional photospheric model VAL C using the radiative transfer code NICOLE. 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 MHD models of magneto-convection.
Results. It is shown that the developed Stokes V widths (SVW) 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 considered lines can also be used for the photospheric field diagnostics with this method, however, 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.
| Original language | English |
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| Journal | Astronomy & Astrophysics |
| Publication status | Accepted/In press - 3 Dec 2019 |