CHIANTI - An atomic database for Emission Lines. Version 8

By G. D. Zanna, K. Dere, Peter R. Young, E. Landi, Helen E. Mason. 2015

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We present version 8 of the CHIANTI database. This version includes a large amount of new data and ions, which represent a significant improvement in the soft X-ray, EUV and UV spectral regions, which several space missions currently cover. New data for neutrals and low charge states are also added. The data are assessed, but to improve the modelling of low-temperature plasma the effective collision strengths for most of the new datasets are not spline-fitted as previously, but are retained as calculated. This required a change of the format of the CHIANTI electron excitation files. The format of the energy files has also been changed. Excitation rates between all the levels are retained for most of the new datasets, so the data can in principle be used to model high-density plasma. In addition, the method for computing the differential emission measure used in the CHIANTI software has been changed.

Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics, Mechanics of Materials

View Paper: https://www.semanticscholar.org/paper/613d61379d5d79415cc1260bfc5133904bb10e90

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Citations in the corpus

CHIANTI—An Atomic Database for Emission Lines. XV. Version 9, Improvements for the X-Ray Satellite Lines (2019, methodology): “In CHIANTI version 8 (Del Zanna et al. 2015) the atomic models for the lithium sequence ions were updated with the collision strengths of Liang & Badnell (2011), which were provided for transitions between all bound levels with a valence electron with n ≤ 5 and core electron excitations up to n = 4.”
Relativistic jet feedback in high-redshift galaxies – I. Dynamics (2016, methodology): “Phys., 54, 174 Collet C. et al., 2016, A&A, 586, A152 Croston J. H., Kraft R. P., Hardcastle M. J., 2007, ApJ, 660, 191 Croston J. H. et al., 2008, A&A, 487, 431 Croton D. J. et al., 2006, MNRAS, 365, 11 Dasyra K. M., Combes F., Novak G. S., Bremer M., Spinoglio L., Pereira Santaella M., Salomé P.,”
Coronal Heating by MHD Waves (2020, methodology): “Using the radiative cooling L(ρ,T ) from the CHIANTI atomic database (Dere et al. 1997, 2019), and a parametrised heating function H(ρ,T ) ∝ ρaT b , Kolotkov et al. (2019) compute numerically the oscillation quality factor q as a function of the heating indices a and b.”