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CHIANTI -- an atomic database for emission lines -- Paper XVI: Version 10, further extensions

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arxiv 2011.05211 v2 pith:4BJMIK64 submitted 2020-11-10 physics.atom-ph astro-ph.SR

G. Del Zanna , K. P. Dere , P. R. Young , E. Landi This is my paper · ORCID
classification physics.atom-phastro-ph.SR
keywords atomicionsseveralversionaddedcalculationschiantiline
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We present version 10 of the CHIANTI package. In this release, we provide updated atomic models for several helium-like ions and for all the ions of the beryllium, carbon and magnesium isoelectronic sequences that are abundant in astrophysical plasmas. We include rates from large-scale atomic structure and scattering calculations that are in many cases a significant improvement over the previous version, especially for the Be-like sequence, which has useful line diagnostics to measure the electron density and temperature. We have also added new ions and updated several of them with new atomic rates and line identifications. Also, we have added several improvements to the IDL software, to speed up the calculations and to estimate the suppression of dielectronic recombination.

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Cited by 3 Pith papers

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