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Chromospheric polarization in the photospheric solar oxygen infrared triplet.
Author/s: T. Del Pino Alemán y J. Trujillo Bueno
Reference: 2015, ApJ, 808, L13 | Link
Figure caption: The Stokes I and Q/I profiles of the IR triplet of O I calculated in the FAL-C semi-empirical model for a line of sight with μ = 0.1. The positive reference direction for Stokes Q is the parallel to the nearest limb. Top panels: the Stokes I profiles normalized to the continuum intensity. Central panels: Q/I profiles calculated with (solid curves) and without (dashed curves) elastic collisions. Bottom panels: Q/I profiles neglecting the contribution of dichroism (dashed curves) and taking it into account (solid curves).
We present multilevel radiative transfer modeling of the scattering polarization observed in the solar O I infrared triplet around 777 nm. We demonstrate that the scattering polarization pattern observed on the solar disk forms in the chromosphere, far above the photospheric region where the bulk of the emergent intensity profiles originate. We investigate the sensitivity of the polarization pattern to the thermal structure of the solar atmosphere and to the presence of weak magnetic fields (0.01 –100 G) through the Hanle effect, showing that the scattering polarization signals of the oxygen infrared triplet encode information on the magnetism of the solar chromosphere.