2013/12/06 by Anna L. H. Hughes, Jack Harvey, Hughes, Anna L. H. +7
Engineering · Physics and Astronomy · #FOS: Physical sciences #Instrumentation and Methods for Astrophysics (astro-ph.IM) #Reservoir Engineering and Simulation Methods #Solar and Stellar Astrophysics (astro-ph.SR) #astro-ph.IM #astro-ph.SR
paper · pdf · doi:10.48550/arxiv.1312.2026
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
openalex publication_date 2013/12/06 · arxiv created 2016/06/16 · arxiv updated 2016/06/17 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
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.