English (United Kingdom)

https://curated-unify.zendy.io/wp-json/zendy-region/v1/featured_content/oa?rat=en

https://curated-unify.zendy.io/wp-json/zendy-region/v1/highlighted_journal/

Global: Zendy Plus annual

Presents the access of premium content as premium feature

Premium Content

Presents the keyphrase highlighting as premium feature

Keyphrase Highlighting

Presents the summarisation as premium feature

Summarisation

Insights

Presents the pdf analysis as premium feature

PDF Analysis

Presents the zaia usage as premium feature

ZAIA

Global: Zendy Plus monthly

Global: Zendy Tools annual

Global: Zendy Tools monthly

Global: Zendy Free Plan

The origin of the activity in the solar corona is a long-standing problem insolar physics. Recent satellite observations, such as Hinode, Solar DynamicsObservatory (SDO), Interface Region Imaging Spectrograph (IRIS), show thedetail characteristics of the solar atmosphere and try to reveal the energytransfer from the photosphere to the corona through the magnetic fields and itsenergy conversion by various processes. However, quantitative estimation ofenergy transfer along the magnetic field is not enough. There are mainly tworeason why it is difficult to observe the energy transfer from photosphere tocorona; 1) spatial resolution gap between photosphere (a few 0.1 arcsec) andcorona (a few arcsec), 2) lack in temperature coverage. Furthermore, there isnot enough observational knowledge of the physical parameters in the energydissipation region. There are mainly three reason why it is difficult toobserve in the vicinity of the energy dissipation region; 1) small spatialscale, 2) short time scale, 3) low emission. It is generally believed that theenergy dissipation occurs in the very small scale and its duration is veryshort (10 second). Further, the density in the dissipation region might be verylow. Therefore, the high spatial and temporal resolution UV/EUV spectroscopicobservation with wide temperature coverage is crucial to estimate the energytransport from photosphere to corona quantitatively and diagnose the plasmadynamics in the vicinity of the energy dissipation region. Main Science Targetfor the telescope is quantitative estimation for the energy transfer from thephotosphere to the corona, and clarification of the plasma dynamics in thevicinity of the energy dissipation region, where is the key region for coronalheating, solar wind acceleration, and/or solar flare, by the high spatial andtemporal resolution UV/EUV spectroscopy.

UV/EUV High-Throughput Spectroscopic Telescope: A Next Generation Solar Physics Mission white paper