CHIANTI – An atomic database for emission lines. Version 8
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TLDR
This version of the CHIANTI database 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.Abstract:
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, extreme UV (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.read more
Citations
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Journal ArticleDOI
Solar UV and X-ray spectral diagnostics
Giulio Del Zanna,Helen E. Mason +1 more
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CHIANTI - an atomic database for emission lines - Paper XV: Version 9, improvements for the X-ray satellite lines
TL;DR: ChiANTI as discussed by the authors contains a large quantity of atomic data for the analysis of astrophysical spectra, including atomic energy levels, wavelengths, radiative transition probabilities, rate coefficients for collisional excitation, ionization, and recombination, as well as data to calculate free-free, free-bound, and two-photon continuum emission.
Journal ArticleDOI
CHIANTI—An Atomic Database for Emission Lines. XV. Version 9, Improvements for the X-Ray Satellite Lines
TL;DR: The Chianti database as mentioned in this paper contains a large quantity of atomic data for the analysis of astrophysical spectra, including energy levels, wavelengths, radiative transition probabilities, rate coefficients for collisional excitation, ionization, and recombination, as well as data to calculate free-free, free-bound and two-photon continuum emission.
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Spectroscopic Observations of Current Sheet Formation and Evolution
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References
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Journal ArticleDOI
CHIANTI - an atomic database for emission lines - I. Wavelengths greater than 50 Å
TL;DR: The CHIANTI database as mentioned in this paper is a set of atomic data and transition probabilities necessary to calculate the emission line spectrum of astrophysical plasmas, including atomic energy levels, atomic radiative data such as wavelengths, weighted oscillator strengths and A values, and electron collisional excitation rates.
Journal ArticleDOI
The Interface Region Imaging Spectrograph (IRIS)
B. De Pontieu,B. De Pontieu,Alan M. Title,James R. Lemen,Gary D. Kushner,D. J. Akin,B. Allard,Thomas E. Berger,Paul Boerner,Mark C. M. Cheung,C. Chou,J. F. Drake,Dexter W. Duncan,Samuel L. Freeland,G. F. Heyman,C. Hoffman,Neal E. Hurlburt,R.W. Lindgren,D. Mathur,R. Rehse,D. Sabolish,R. Seguin,Carolus J. Schrijver,Theodore D. Tarbell,J. P. Wülser,C. J. Wolfson,C. Yanari,Jason Mudge,N. Nguyen-Phuc,R. Timmons,R. van Bezooijen,I. Weingrod,R. Brookner,G. Butcher,B. Dougherty,J. Eder,V. Knagenhjelm,S. Larsen,D. Mansir,L. Phan,P. Boyle,Peter Cheimets,Edward E. DeLuca,Leon Golub,Richard Gates,Edward Hertz,S. McKillop,Sung-Hong Park,T. Perry,William A. Podgorski,Katharine K. Reeves,Steven H. Saar,Paola Testa,Hui Tian,M. A. Weber,C. Dunn,S. Eccles,S. Jaeggli,Charles C. Kankelborg,K. Mashburn,N. Pust,L. Springer,R. Carvalho,Lucia Kleint,J. Marmie,E. Mazmanian,Tiago M. D. Pereira,Tiago M. D. Pereira,S. Sawyer,J. Strong,Simon P. Worden,Mats Carlsson,Viggo Hansteen,Jorrit Leenaarts,M. Wiesmann,J. Aloise,K.-C. Chu,R. I. Bush,Philip H. Scherrer,P. Brekke,J. Martinez-Sykora,Bruce W. Lites,Scott W. McIntosh,Han Uitenbroek,Takenori J. Okamoto,M. A. Gummin,G. Auker,P. Jerram,Peter J. Pool,N. Waltham +89 more
TL;DR: The Interface Region Imaging Spectrograph (IRIS) as mentioned in this paper provides simultaneous spectra and images of the photosphere, chromosphere, transition region, and corona with 0.33 arcsec and up.
Journal ArticleDOI
The flexible atomic code
TL;DR: In this paper, a complete software package for the computation of various atomic data such as energy levels; radiative transition; collisional excitation; ionization by electron impact, photoionizatio...
Journal ArticleDOI
The Interface Region Imaging Spectrograph (IRIS)
B. De Pontieu,A. M. Title,James R. Lemen,Gary D. Kushner,D. J. Akin,B. Allard,Thomas E. Berger,Paul Boerner,Mark C. M. Cheung,C. Chou,J. F. Drake,Dexter W. Duncan,Samuel L. Freeland,G. F. Heyman,C. Hoffman,Neal E. Hurlburt,R.W. Lindgren,D. Mathur,R. Rehse,D. Sabolish,R. Seguin,Carolus J. Schrijver,T. D. Tarbell,Jean-Pierre Wuelser,C. J. Wolfson,C. Yanari,Jason Mudge,N. Nguyen-Phuc,R. Timmons,R. van Bezooijen,I. Weingrod,R. Brookner,G. Butcher,B. Dougherty,J. Eder,V. Knagenhjelm,S. Larsen,D. Mansir,L. Phan,P. Boyle,Peter Cheimets,Edward E. DeLuca,Leon Golub,Richard Gates,Edward Hertz,Sean McKillop,Sung-Hong Park,T. Perry,William A. Podgorski,Katharine K. Reeves,S. H. Saar,Paola Testa,Hui Tian,M. Weber,C. Dunn,S. Eccles,S. Jaeggli,Charles C. Kankelborg,K. Mashburn,N. Pust,L. Springer,R. Carvalho,Lucia Kleint,J. Marmie,E. Mazmanian,Tiago M. D. Pereira,S. Sawyer,J. Strong,Simon P. Worden,Mats Carlsson,Viggo Hansteen,Jorrit Leenaarts,M. Wiesmann,J. Aloise,K.-C. Chu,R. I. Bush,Philip H. Scherrer,P. Brekke,Juan Martinez-Sykora,Bruce W. Lites,Scott W. McIntosh,Han Uitenbroek,Takenori J. Okamoto,M. A. Gummin,G. Auker,P. Jerram,Peter J. Pool,N. Waltham +87 more
TL;DR: The Interface Region Imaging Spectrograph (IRIS) as mentioned in this paper is a small explorer spacecraft that provides simultaneous spectra and images of the photosphere, chromosphere, transition region, and corona with 0.33-0.4 arcsec spatial resolution, 2 s temporal resolution and 1 km/s velocity resolution over a field-of-view of up to 175 arcsec.
Journal ArticleDOI
Chianti—an atomic database for emission lines. xiii. soft x-ray improvements and other changes
TL;DR: The CHIANTI spectral code as mentioned in this paper 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 the astrophysical spectra.
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