Chromospheric polarimetry through multi-line observations of the 850 nm spectral region

Abstract

Future solar missions and ground-based telescopes aim to understand the magnetism of the solar chromosphere. We performed a supporting study in Quintero Noda et al. (2016) focused on the infrared Ca II 8542 A line and we concluded that is one of the best candidates because it is sensitive to a large range of atmospheric heights, from the photosphere to the middle chromosphere. However, we believe that it is worth to try improving the results produced by this line observing additional spectral lines. In that regard, we examined the neighbour solar spectrum looking for spectral lines that could increase the sensitivity to the atmospheric parameters. Interestingly, we discovered several photospheric lines that greatly improve the photospheric sensitivity to the magnetic field vector. Moreover, they are located close to a second chromospheric line that also belongs to the Ca II infrared triplet, i.e. the Ca II 8498 A line, and enhances the sensitivity to the atmospheric parameters at chromospheric layers. We conclude that the lines in the vicinity of the Ca II 8542 A line not only increase its sensitivity to the atmospheric parameters at all layers, but also they constitute an excellent spectral window for chromospheric polarimetry.

arXiv comment11 pages, 8 figures, 1 table

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Cited by in corpus (21)

• Spectropolarimetric NLTE inversion code SNAPI
• DeSIRe: Departure coefficient aided Stokes Inversion based on Response functions
• On the weak field approximation for CaII 8542 A
• Temperature constraints from inversions of synthetic solar optical, UV and radio spectra
• Sunrise III: Overview of Observatory and Instruments
• Solar polarimetry through the K I lines at 770 nm
• Comparison of Two Coronal Magnetic Field Models for Reconstructing a Sigmoidal Solar Active Region With Coronal Loops
• The potential of many-line inversions of photospheric spectropolarimetric data in the visible and near UV
• Diagnostic capabilities of spectropolarimetric observations for understanding solar phenomena I. Zeeman-sensitive photospheric lines
• Study of the polarization produced by the Zeeman effect in the solar Mg I b lines
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• Height dependence of the penumbral fine-scale structure in the inner solar atmosphere
• Spectropolarimetric Fluctuations in a Sunspot Chromosphere
• Chromospheric polarimetry through multi-line observations of the 850 nm spectral region III: Chromospheric jets driven by twisted magnetic fields
• The Sunrise Chromospheric Infrared Spectro-Polarimeter SCIP: an instrument for SUNRISE III
• Developments of Multi-wavelength Spectro-Polarimeter on the Domeless Solar Telescope at Hida Observatory
• Understanding the thermal and magnetic properties of a X-class flare in the low solar atmosphere
• Development of Fast and Precise Scan Mirror Mechanism for an Airborne Solar Telescope
• Episodic Plasma Flows and Coronal Brightenings in an Arch Filament System Observed with SUNRISE III
• On the (mis)interpretation of the scattering polarization signatures in the Ca II 8542 A line through spectral line inversions
• Effects of spatial resolution on inferences of atmospheric quantities from simulations