期刊
ASTROPHYSICAL JOURNAL
卷 763, 期 2, 页码 -出版社
IOP PUBLISHING LTD
DOI: 10.1088/0004-637X/763/2/86
关键词
atomic data; atomic processes; Sun: UV radiation; Sun: X-rays, gamma rays; ultraviolet: general; X-rays: general
资金
- NSF [AGS-1154443]
- STFC via the Advanced Fellowship program
- UK APAP Network
- NASA [NNX11AC20G]
- STFC
- [NNX10AQ58G NASA]
- Directorate For Geosciences [1154443] Funding Source: National Science Foundation
- Div Atmospheric & Geospace Sciences [1154443] Funding Source: National Science Foundation
- Science and Technology Facilities Council [ST/J001570/1, ST/J000892/1, PP/E004857/2] Funding Source: researchfish
- STFC [PP/E004857/2, ST/J000892/1, ST/J001570/1] Funding Source: UKRI
The CHIANTI spectral code consists of two parts: an atomic database and a suite of computer programs in Python and IDL. Together, they allow the calculation of the optically thin spectrum of astrophysical objects and provide spectroscopic plasma diagnostics for the analysis of astrophysical spectra. The database includes atomic energy levels, wavelengths, radiative transition probabilities, collision excitation rate coefficients, ionization, and recombination rate coefficients, as well as data to calculate free-free, free-bound, and two-photon continuum emission. Version 7.1 has been released, which includes improved data for several ions, recombination rates, and element abundances. In particular, it provides a large expansion of the CHIANTI models for key Fe ions from Fe VIII to Fe XIV to improve the predicted emission in the 50-170 angstrom wavelength range. All data and programs are freely available at http://www.chiantidatabase.org and in SolarSoft, while the Python interface to CHIANTI can be found at http://chiantipy.sourceforge.net.
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