Speaker
Description
The solar chromosphere is one of the most intriguing yet poorly understood regions of the solar atmosphere, and its heating remains a central problem in solar physics. Plage regions, characterized by the strong, predominantly vertical magnetic fields, show enhanced chromospheric emission, indicating localized energy deposition. The dominant
mechanisms that heat the chromosphere include waves, magnetic reconnection, and magnetic braiding. Mass motions, such as vortex flows, may also contribute to the chromospheric heating. Overall, both observations and simulations indicate that multiple processes operate simultaneously, producing a complex, spatially heterogeneous
heating pattern. The dominant process heating the chromosphere within plages remains an open question.
We plan to use multi-line, high-resolution spectropolarimetric observations from Sunrise III to investigate the processes that heat the chromosphere in plage regions. The idea is to perform spectropolarimetric inversions of the Ca II observations from SUSI and/or SCIP data using the STiC inversion code. The inversions, applied to the datasets with
high spectral resolution and coverage, will enable detailed optical-depth resolution of the inverted atmosphere, helping accurately constrain the radiative losses that will be constrained with an estimate of the Poynting flux derived from the spatio-temporally resolved TuMag observations. The comparison between the two will provide a unique, multi-instrument, multi-layered insight into energy transport within the solar plages.