Zeemanfit: Use and Development of the solis_vms_zeemanfit code
Abstract
The purpose of the SOLIS Zeemanfit Code is to provide a straight-forward, easily checked measure of the total magnetic-field strength in the high-strength umbral regions of the solar disk. In the highest-strength regions, the Zeeman splitting of the 6302-angstrom Fe line becomes wide enough for the triplet nature of the line to be visible by eye in non-polarized light. Therefore, a three-line fit to the spectra should, in principle, provide a fairly robust measure of the total magnetic-field strength. The code uses the Level-1.5 spec-cube data of the SOLIS VSM 6302-vector observations (specifically the Stokes-I and Stokes-V components) to fit the line profiles at each appropriate pixel and calculate the magnetic-field-strength from the line-center separation of the two fit 6302.5 sigma-components. The 6301.5-angstrom Fe line is also present and fit in the VSM 6302-vector data, but it is an anomalous-Zeeman line with a weaker response to magnetic fields. Therefore, no magnetic- field measure is derived from this portion of the spectral fit.
Keywords
Cite
@article{arxiv.1312.2026,
title = {Zeemanfit: Use and Development of the solis_vms_zeemanfit code},
author = {Anna L. H. Hughes and Jack Harvey and Andrew R. Marble and Alexei A. Pevtsov},
journal= {arXiv preprint arXiv:1312.2026},
year = {2016}
}
Comments
39 pages containing 30 figures. Represents the primary documentation for the new SOLIS VSM Zeemanfit data product; corrected confusing variable units listed below Equation 9