2014/02/10 by Antonino Petralia, A. Petralia, F. Reale +3 · 20 citations
Physics and Astronomy · #Astro and Planetary Science #Astrobiology #Astronomy #Astrophysics #Corona (planetary geology) #Extreme ultraviolet #Extreme ultraviolet lithography #Imaging spectrometer #Line (geometry) #Line-of-sight #Meteorology #Observatory #Optics #Physics #Plasma #Solar and Space Plasma Dynamics #Solar flare #Spectrometer #Stellar, planetary, and galactic studies #Thermal #Ultraviolet #astro-ph.SR
paper · pdf · doi:10.1051/0004-6361/201322998
published in Astronomy and Astrophysics 564, A3 (EDP Sciences) · 12 pages, 8 figures, accepted for publication
openalex publication_date 2014/02/10 · arxiv created 2014/02/26 · arxiv updated 2015/06/18 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Aims. In previous studies, a very hot plasma component has been diagnosed in solar active regions through the images in three different narrow-band channels of Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory (SDO). This diagnostic from extreme ultraviolet (EUV) imaging data has also been supported by the matching morphology of emission in the hot Ca XVII line, as observed with Extreme-Ultraviolet Imaging Spectrometer (EIS) on board Hinode. This evidence is debated because of the unknown distribution of the emission measure along the line of sight. Here we investigate in detail the thermal distribution of one such region using EUV spectroscopic data.