CHIANTI—AN ATOMIC DATABASE FOR EMISSION LINES. XII. VERSION 7 OF THE DATABASE
By E. Landi, G. D. Zanna, Peter R. Young, K. Dere, Helen E. Mason. 2012
260 citations recorded by the source corpus.
Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Mechanics of Materials
View Paper: https://www.semanticscholar.org/paper/9f37bd6500bcc8ed946c0fd3dc9deb6334c24c12
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Citations in the corpus
- UPDATED ATOMIC DATA AND CALCULATIONS FOR X-RAY SPECTROSCOPY (2012, unknown): “0 (Kaastra et al. 1996), CHIANTI v7 (Landi et al. 2012) and AtomDB v1.”
- HIGH-DENSITY CIRCUMSTELLAR INTERACTION IN THE LUMINOUS TYPE IIn SN 2010jl: THE FIRST 1100 DAYS (2013, methodology): “For the collision strengths and radiative transition rates we use data from the Chianti data base (Landi et al. 2012).”
- Survival of molecular gas in cavities of transition disks - I. CO (2013, unknown): “Chianti = Dere et al. (1997) and Landi et al. (2012).”
- NEW STRONG-LINE ABUNDANCE DIAGNOSTICS FOR H ii REGIONS: EFFECTS OF κ-DISTRIBUTED ELECTRON ENERGIES AND NEW ATOMIC DATA (2013, methodology): “The temperature coordinates were normalized in a fashion similar to that used in CHIANTI 7.1 (Dere et al. 1997; Landi et al. 2012) and originally proposed by Burgess & Tully (1992), but here we use a more direct scaled temperature coordinate x = T/(T +TC), where T is the temperature and TC is a…”
- CHIANTI—An Atomic Database for Emission Lines. XV. Version 9, Improvements for the X-Ray Satellite Lines (2019, methodology): “Mn X The Mn X model was added to CHIANTI 7 (Landi et al. 2012) and featured 48 fine structure levels.”
- CHIANTI - An atomic database for Emission Lines. Version 8 (2015, methodology): “Landi et al. (2012) provided the first published description of the ChiantiPy7 software.”
- EXTENSION OF THE MURAM RADIATIVE MHD CODE FOR CORONAL SIMULATIONS (2016, methodology): “For the function Λ(T ) we use a tabulated loss function taken from CHIANTI 7 with photospheric abundances Landi et al. (2012).”
- Origins of the Ambient Solar Wind: Implications for Space Weather (2017, methodology): “However, Landi et al. (2012a) suggested that the relative fractions of carbon ions C+4, C+5, and C+6 may be more precise probes of the plasma conditions in the low corona (r ≈ 1.2R ) where the freezing-in occurs.”