Solar Physics and the Solar-Stellar Connection at Dome C

TL;DR

This paper discusses the advantages of Dome C's unique observational conditions for studying solar magnetic field evolution and introduces new instruments and science cases for solar and stellar observations in this environment.

Contribution

It presents the Advanced Solar Photometric Imager and Radiation Experiment and explores the potential of the International Concordia Explorer Telescope for solar-stellar research at Dome C.

Findings

Dome C offers continuous excellent seeing conditions for solar observations.

The proposed instruments can address key questions in solar magnetic field evolution.

Science cases include synoptic solar monitoring and solar-stellar connection studies.

Abstract

Solar magnetic fields evolve on many time-scales, e.g., the generation, migration, and dissipation of magnetic flux during the 22-year magnetic cycle of the Sun. Active regions develop and decay over periods of weeks. The build-up of magnetic shear in active regions can occur within less than a day. At the shortest time-scales, the magnetic field topology can change rapidly within a few minutes as the result of eruptive events such as flares, filament eruptions, and coronal mass ejections. The unique daytime seeing characteristics at Dome C, i.e., continuous periods of very good to excellent seeing during almost the entire Antarctic summer, allow us to address many of the top science cases related to the evolution of solar magnetic fields. We introduce the Advanced Solar Photometric Imager and Radiation Experiment and present the science cases for synoptic solar observations at Dome C. Furthermore, common science cases concerning the solar-stellar connection are discussed in the context of the proposed International Concordia Explorer Telescope.