High Resolution Soft X-ray Spectroscopy and the Quest for the Hot (5–10 MK) Plasma in Solar Active Regions

Frontiers in Astronomy and Space Sciences

Helen E. Mason¹  Giulio Del Zanna¹  Leon Golub²  Vincenzo Andretta³  James A. Klimchuk⁴  Adrian N. Daw⁴  Alain J. Corso⁵  Peter J. Cargill⁶ 

[1] Department of Applied Mathematics and Theoretical Physics, University of Cambridge, Cambridge, United Kingdom;Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, United States;Istituto Nazionale di Astrofisica, Osservatorio Astronomico di Capodimonte, Naples, Italy;NASA Goddard Space Flight Center, Greenbelt, MD, United States;National Research Council-Institute for Photonics and Nanotechnologies, Padova, Italy;Space and Atmospheric Physics, The Blackett Laboratory, Imperial College London, London, United Kingdom;School of Mathematics and Statistics, University of St Andrews, St Andrews, United Kingdom;

关键词: sun–active regions;    sun–atmosphere;    X-ray;    spectroscopy;    coronal heating;   

DOI  :  10.3389/fspas.2021.638489

来源: Frontiers

【 摘 要 】

We discuss the diagnostics available to study the 5–10 MK plasma in the solar corona, which is key to understanding the heating in the cores of solar active regions. We present several simulated spectra, and show that excellent diagnostics are available in the soft X-rays, around 100 Å, as six ionization stages of Fe can simultaneously be observed, and electron densities derived, within a narrow spectral region. As this spectral range is almost unexplored, we present an analysis of available and simulated spectra, to compare the hot emission with the cooler component. We adopt recently designed multilayers to present estimates of count rates in the hot lines, with a baseline spectrometer design. Excellent count rates are found, opening up the exciting opportunity to obtain high-resolution spectroscopy of hot plasma.

【 授权许可】

CC BY