2010/07/01 by M. M. Sirk, Martin Sirk, Mark Hurwitz +3 · 8 citations
Physics and Astronomy · #Astrophysics and Star Formation Studies #Cosmic ray #Emission spectrum #Extreme ultraviolet lithography #Interstellar medium #Isothermal process #Plasma #Solar and Space Plasma Dynamics #Spectral line #Spectrometer #Stellar, planetary, and galactic studies #astro-ph.SR #physics.plasm-ph
paper · pdf · doi:10.1007/s11207-010-9591-7
published in Solar Physics 264(2), 287-309 (Springer Science+Business Media) · 27 Pages, 13 Figures
openalex publication_date 2010/07/01 · arxiv created 2010/07/14 · arxiv updated 2010/07/16 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We analyze EUV spectra of the full solar disk from the Cosmic Hot Interstellar Plasma Spectrometer (CHIPS) spanning a period of two years. The observations were obtained via a fortuitous off-axis light path in the 140 – 275 Å passband. The general appearance of the spectra remained relatively stable over the two-year time period, but did show significant variations of up to 25% between two sets of Fe lines that show peak emission at 1 MK and 2 MK. The variations occur at a measured period of 27.2 days and are caused by regions of hotter and cooler plasma rotating into, and out of, the field of view. The CHIANTI spectral code is employed to determine plasma temperatures, densities, and emission measures. A set of five isothermal plasmas fit the full-disk spectra well. A 1 – 2 MK plasma of Fe contributes 85% of the total emission in the CHIPS passband. The standard Differential Emission Measures (DEMs) supplied with the CHIANTI package do not fit the CHIPS spectra well as they over-predict emission at temperatures below log 10 T=6.0 and above log 10 T=6.3. The results are important for cross-calibrating TIMED, SORCE, SOHO/EIT, and CDS/GIS, as well as the recently launched Solar Dynamics Observatory.