J. Lang

TL;DR: The Extreme-UV Imaging Spectrometer (EISASV) was used in the ISAS/JAXA Solar-B mission as mentioned in this paper to detect photons in the wavelength ranges 17 - 21 nm and 25 - 29 nm.

TL;DR: In this paper, the authors presented and discussed spectra obtained by SUMER on SOHO from an active region loop system ob- served on the solar disc, close to the central meridian, on July 26th, 1996.

TL;DR: In this paper, the spectral lines of highly ionized ions of sulfur, calcium, and iron that appear in solar flare spectra were used to determine the electron temperature independently of the assumption of ionization equilibrium, and an attempt was made to find emission measure models based on selected functional dependences of emission measure on temperature.

TL;DR: Theoretical populations of the 2s3l levels of the solar spectrum for electron temperatures from 2.5 × 105 K to 4 × 106 K and electron densities from 108 cm −3 to 1012 cm−3 were presented in this article, in conjunction with intensities of previously observed solar Ne vii lines and wavelengths and intensities observed in the laboratory.

TL;DR: The Fe K-alpha and K-beta X-ray lines (wavelengths 1.94 and 1.76 A) are formed by fluoroescence of photospheric iron atoms, and the ratio of the intensity of either to the He-like iron (Fe XXV) resonance line at 1.85 A is a function of the photosphereto-coronal abundance of iron.