コンビーナ:今田 晋亮(名古屋大学宇宙地球環境研究所)、Alphonse Sterling(NASA/MSFC)、横山 央明(東京大学大学院理学系研究科)、清水 敏文(宇宙航空研究開発機構宇宙科学研究所)

Over recent decades, Sun-observing satellite missions have told us much about the dynamic solar atmosphere. These satellites can observe magnetic activity in the solar corona at wavelengths inaccessible from ground-based telescopes, such as X-rays and EUV. Additionally, the seeing-free conditions of space allow for consistent, high-spatial resolution at visible wavelengths; e.g. the HInode satellite can observe solar surface magnetic field elements down to ~0.2 arcsec. From observations such as these, we have identified three important points regarding what is required form future space-based solar missions to solve fundamental solar problems, such as how the corona is heated and what drives solar eruptions: (1) seamless observation over all temperature regimes of the solar atmosphere, from the chromosphere to the corona, at the same time; (2) high spatial and temporal resolution to resolve elemental structures of the solar atmosphere, and to track their evolution; and (3) plasma diagnostic capability to quantify the dynamics of elementary process taking place in the solar atmosphere. To meet these requirements, recently the solar physics community in Japan proposed the Solar-C_EUVST mission, which will be launched in the mid-2020s. Furthermore, additional top-rate solar observatories, such as the Parker Solar Probe (PSP), Solar Orbiter, and the Daniel K. Inouye Solar Telescope (DKIST), will be operating in the years leading up to Solar-C_EUVST. In this session we will discuss what solar physics observational and numerical-simulation studies are required prior to the mid-2020s, to prepare most efficiently for the new observational era. We welcome contributions dealing with remote-sensing space-based observations (e.g. from Hinode and SDO), in-situ observations from near- and deep-space (e.g., PSP, Pioneer), ground-based observations, and numerical studies.