TIC: A Stokes inversion code for scattering polarization with partial frequency redistribution and arbitrary magnetic fields

Abstract

We present the Tenerife Inversion Code (TIC), which has been developed to infer the magnetic and plasma properties of the solar chromosphere and transition region via full-Stokes inversion of polarized spectral lines. The code is based on the HanleRT forward engine, which takes into account many of the physical mechanisms that are critical for a proper modeling of the Stokes profiles of spectral lines originating in the tenuous and highly dynamic plasmas of the chromosphere and transition region: quantum level population imbalance and interference (atomic polarization), frequency coherence effects in polarized resonance scattering (partial frequency redistribution), and the impact of arbitrary magnetic fields on the atomic polarization and the radiation field. We present first results of atmospheric and magnetic inversions, and discuss future developments for the project.

17pages, 7 figures. Accepted for publication in The Astrophysical Journal

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Cited by in corpus (12)

• The European Solar Telescope
• Tomography of a solar plage with the Tenerife Inversion Code
• Optimal spectral lines for measuring chromospheric magnetic fields
• Effects of spectral resolution on simple magnetic field diagnostics of the Mg II h & k lines
• Combining magneto-hydrostatic constraints with Stokes profiles inversions. III. Uncertainty in the inference of electric currents
• Evidence for the Operation of the Hanle and Magneto-Optical Effects in the Scattering Polarization Signals Observed by CLASP2 Across the Mg II h and k Lines
• Determining the Magnetic Field in the Atmosphere of a Solar Active Region Observed by the CLASP2.1 Sounding Rocket Experiment
• A numerical approach for modelling the polarisation signals of strong resonance lines with partial frequency redistribution. Numerical applications to two-term atoms and plane-parallel atmospheres
• Non-Local Thermodynamic Equilibrium inversions of the Si I 10827 A spectral line
• Derivation of Instrument Requirements for Polarimetry using Mg, Fe, and Mn lines between 250 and 290 nm
• The magnetic sensitivity of the Ca II resonance and subordinate lines in the solar atmosphere
• The magnetic sensitivity of the Ca II H and K lines