Title: UV/EUV High-Throughput Spectroscopic Telescope: A Next Generation Solar Physics Mission white paper,
Abstract: The origin of the activity in the solar corona is a long-standing problem in
solar physics. Recent satellite observations, such as Hinode, Solar Dynamics
Observatory (SDO), Interface Region Imaging Spectrograph (IRIS), show the
detail characteristics of the solar atmosphere and try to reveal the energy
transfer from the photosphere to the corona through the magnetic fields and its
energy conversion by various processes. However, quantitative estimation of
energy transfer along the magnetic field is not enough. There are mainly two
reason why it is difficult to observe the energy transfer from photosphere to
corona; 1) spatial resolution gap between photosphere (a few 0.1 arcsec) and
corona (a few arcsec), 2) lack in temperature coverage. Furthermore, there is
not enough observational knowledge of the physical parameters in the energy
dissipation region. There are mainly three reason why it is difficult to
observe in the vicinity of the energy dissipation region; 1) small spatial
scale, 2) short time scale, 3) low emission. It is generally believed that the
energy dissipation occurs in the very small scale and its duration is very
short (10 second). Further, the density in the dissipation region might be very
low. Therefore, the high spatial and temporal resolution UV/EUV spectroscopic
observation with wide temperature coverage is crucial to estimate the energy
transport from photosphere to corona quantitatively and diagnose the plasma
dynamics in the vicinity of the energy dissipation region. Main Science Target
for the telescope is quantitative estimation for the energy transfer from the
photosphere to the corona, and clarification of the plasma dynamics in the
vicinity of the energy dissipation region, where is the key region for coronal
heating, solar wind acceleration, and/or solar flare, by the high spatial and
temporal resolution UV/EUV spectroscopy.