A NEW APPROACH TO ANALYZING SOLAR CORONAL SPECTRA AND UPDATED COLLISIONAL IONIZATION EQUILIBRIUM CALCULATIONS. II. UPDATED IONIZATION RATE COEFFICIENTS
By P. Bryans, E. Landi, D. Savin. 2008
196 citations recorded by the source corpus.
We have re-analyzed Solar Ultraviolet Measurement of Emitted Radiation (SUMER) observations of a parcel of coronal gas using new collisional ionization equilibrium (CIE) calculations. These improved CIE fractional abundances were calculated using state-of-the-art electron–ion recombination data for K-shell, L-shell, Na-like, and Mg-like ions of all elements from H through Zn and, additionally, Al- through Ar-like ions of Fe. They also incorporate the latest recommended electron impact ionization data for all ions of H through Zn. Improved CIE calculations based on these recombination and ionization data are presented here. We have also developed a new systematic method for determining the average emission measure (EM) and electron temperature (Te) of an isothermal plasma. With our new CIE data and a new approach for determining average EM and Te, we have re-analyzed SUMER observations of the solar corona. We have compared our results with those of previous studies and found some significant differences for the derived EM and Te. We have also calculated the enhancement of coronal elemental abundances compared to their photospheric abundances, using the SUMER observations themselves to determine the abundance enhancement factor for each of the emitting elements. Our observationally derived first ionization potential factors are in reasonable agreement with the theoretical model of Laming.
Subfields: Astronomy and Astrophysics
View Paper: https://www.semanticscholar.org/paper/dee960591f2263f32f07ae229230c8300ed6dd73
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In Astronomy and Astrophysics
Citations in the corpus
- The FIP and Inverse FIP Effects in Solar and Stellar Coronae (2015, methodology): “, 2010, consider O, Ne, and Fe), and appears unlikely to be able to get every element right at the same time, even if the atmosphere was sufficiently quiescent (see also Byhring et al., 2011; Byhring, 2011). Bøet al. (2013) make the point that above the chromospheric temperature minimum, the atmosph”
- UPDATED ATOMIC DATA AND CALCULATIONS FOR X-RAY SPECTROSCOPY (2012, methodology): “In their papers Bryans et al. (2006, 2009) compare the electron-impact ionization (EII) and recombination data with earlier data sets and with experimental measurements.”