Stoke'sparameters的模擬研究

Solar magnetic fields are dominant driver of observed activities on the Sun. Tounderstand their evolution, dynamics and effects, various models have beendeveloped. To verify these models, their predictions have to be compared withthe observations. Currently, the most commonly used quantity to verify themodels is the magnetic fields on the photosphere. However, they are, in fact, notdirectly observed, but are computed from the directly observedspectropolarimetric spectral profiles, the Stoke’s parameters. The Stoke’sparameters are a set of four parameters that can fully describe the intensity andpolarization of light. The inference of the magnetic fields from the Stoke’sparameters have been computed using inversion methods. However, thesemethods cannot completely extract of all the detailed information contained in theobserved spectral profiles, and the inferred magnetic fields are limited by thespatial resolution of the detector, which is significantly insufficient to resolvesmall-scale magnetic structures, such as quiet Sun network and penumbrafilaments. Earlier studies have demonstrated the potential of using Stoke’s profileto probe these sub-pixel structures and plasma dynamics. In this study, theobjective is to characterize the line properties of Stoke’s profiles in response todifferent model structures. A statistical analysis will be conducted to connect thestatisticalcharacteristics of the response of the profiles to the underlying physicalmechanism and structures. This would improve our understanding andinterpretation of the observed Stoke’s profiles, and pave the way for a directcomparison between the observed and model predicted profiles, which shallenable more accurate validation of the theoretical models.