Journal ArticleDOI
Chianti—an atomic database for emission lines. xiii. soft x-ray improvements and other changes
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TLDR
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.Abstract:
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 A 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.read more
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Journal ArticleDOI
CHIANTI – An atomic database for emission lines. Version 8
TL;DR: 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.
Journal ArticleDOI
Alfvén wave solar model (AWSoM): Coronal heating
B. van der Holst,Igor V. Sokolov,Xing Meng,Meng Jin,Ward B. Manchester,Gabor Toth,Tamas I. Gombosi +6 more
TL;DR: In this paper, a new version of the Alfven wave solar model is presented, which does not impose open-closed magnetic field boundaries; those develop self-consistently.
Journal ArticleDOI
Alfven Wave Solar Model (AWSoM): Coronal Heating
Bart van der Holst,Igor V. Sokolov,Xing Meng,Meng Jin,Ward B. Manchester,Gabor Toth,Tamas I. Gombosi +6 more
TL;DR: In this article, a new version of the AWSoM model is presented, which employs three different temperatures, namely the isotropic electron temperature and the parallel and perpendicular ion temperatures.
Journal ArticleDOI
CHIANTI - An atomic database for Emission Lines. Version 8
TL;DR: The CHIANTI database has been updated in this paper with 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.
Journal ArticleDOI
Thermal diagnostics with the atmospheric imaging assembly on board the solar dynamics observatory: a validated method for differential emission measure inversions
Mark C. M. Cheung,P. Boerner,Carolus J. Schrijver,Paola Testa,Feng Chen,Hardi Peter,A. V. Malanushenko +6 more
TL;DR: In this paper, a method for performing differential emission measure (DEM) inversions on narrow-band EUV images from the Atmospheric Imaging Assembly (AIA) on board the Solar Dynamics Observatory is presented.
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 EUV Imaging Spectrometer for Hinode
J. L. Culhane,Louise K. Harra,A. M. James,K. Al-Janabi,L. Bradley,Rifat A Chaudry,Kerrin Rees,J. Tandy,P. D. Thomas,M. C. R. Whillock,Berend Winter,George A. Doschek,Clarence M. Korendyke,Charles M. Brown,S. H. Myers,J. T. Mariska,John F. Seely,J. Lang,B. J. Kent,B. M. Shaughnessy,Peter R. Young,G. M. Simnett,C. M. Castelli,S. Mahmoud,H. Mapson-Menard,Brian J. Probyn,Roger J. Thomas,Joseph M. Davila,Kenneth P. Dere,David L. Windt,John Shea,R. Hagood,Robert W. Moye,Hirohisa Hara,Takashi Watanabe,K. Matsuzaki,Takeo Kosugi,Viggo Hansteen,Ø. Wikstol +38 more
TL;DR: The EUV Imaging Spectrometer (EIS) as mentioned in this paper is a two-element, normal incidence design with a backside-illuminated, thinned CCD, which has a significantly greater effective area than previous orbiting EUV spectrographs with typical active region 2 -5 s exposure times in the brightest lines.
Journal ArticleDOI
Solar Chemical Abundances Determined with a CO5BOLD 3D Model Atmosphere
TL;DR: In this paper, the photospheric solar metallicity as determined from spectroscopy experienced a remarkable downward revision due to an improvement of atomic data and the inclusion of NLTE computations, but also the use of hydrodynamical model atmospheres.
Journal ArticleDOI
CHIANTI - an atomic database for emission lines. IX. Ionization rates, recombination rates, ionization equilibria for the elements hydrogen through zinc and updated atomic data
TL;DR: The CHIANTI database as mentioned in this paper provides a set of atomic data for the interpretation of astrophysical spectra emitted by collisionally dominated, high temperature, optically thin sources.
Journal ArticleDOI
CHIANTI-An Atomic Database for Emission Lines. VII. New Data for X-Rays and Other Improvements
TL;DR: The CHIANTI atomic database as mentioned in this paper contains atomic energy levels, wavelengths, radiative transition probabilities, and collisional excitation data for a large number of ions of astrophysical interest.
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