VFISV Inversion Code Documentation for SOLIS/VSM Pipeline Implementation

TL;DR

This paper details the implementation of the VFISV inversion code within the SOLIS/VSM pipeline, enabling efficient interpretation of spectropolarimetric data using a Milne-Eddington model for solar magnetic field analysis.

Contribution

It provides a comprehensive documentation of the VFISV inversion code tailored for the SOLIS/VSM pipeline, enhancing reproducibility and understanding of the spectral line inversion process.

Findings

Efficient inversion of Stokes profiles using VFISV in the SOLIS/VSM pipeline.

Accurate inference of magnetic field properties from Fe I lines at 6301.5 and 6302.5 Angstroms.

Implementation details improve reproducibility and usability of the inversion code.

Abstract

Spectral line inversion codes are tools used to interpret spectropolarimetric data; in general, their function is to analyze a set of observed Stokes profiles, and infer the physical properties of the line-formation region in which the Stokes profiles were formed. For the SOLIS/VSM 6302v pipeline, the inversion is based on a Milne-Eddington model atmosphere, optimized to reproduce the observed Stokes profiles of both Fe I lines at 6301.5 and 6302.5 Angstroms . This document provides a detailed overview of the SOLIS/VSM remix of the VFISV (Very Fast Inversion of the Stokes Vector) inversion code, as it is implemented in the SOLIS/VSM pipeline environment.