CHIANTI—An Atomic Database for Emission Lines. VII. New Data for X-Rays and Other Improvements

By E. Landi, G. D. Zanna, Peter R. Young, K. Dere, Helen E. Mason, M. Landini. 2006

397 citations recorded by the source corpus.

Subfields: Atomic and Molecular Physics, and Optics, Mechanics of Materials, Radiation

View Paper: https://www.semanticscholar.org/paper/10746ce62198ae685c176b86358ef781ad3de1bf

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Citations in the corpus

Flows and Nonthermal Velocities in Solar Active Regions Observed with the EUV Imaging Spectrometer on Hinode: A Tracer of Active Region Sources of Heliospheric Magnetic Fields? (2008, background): “5.2) atomic database (e.g., Landi et al. 2006).”
CHIANTI—An Atomic Database for Emission Lines. XV. Version 9, Improvements for the X-Ray Satellite Lines (2019, methodology): “Prior to CHIANTI 9 the radiative recombination rates were implemented as a post-processing step once the level population equations of the standard CHIANTI model had been solved, as described in Landi et al. (2006).”
SEMIEMPIRICAL MODELS OF THE SOLAR ATMOSPHERE. III. SET OF NON-LTE MODELS FOR FAR-ULTRAVIOLET/EXTREME-ULTRAVIOLET IRRADIANCE COMPUTATION (2009, methodology): “Previous transition region models describe the differential emission measure (DEM; e.g., Monsignori Fossi & Landini 1992) as a function of temperature and are found in the CHIANTI 5.2 (Dere et al. 1997; Landi et al. 2006) collection of data.”
Ionization rate coefficients for the elements hydrogen through zinc (2007, methodology): “Further, the cross sections and rate coefficients will be available through the CHIANTI atomic database for astrophysical spectroscopy Dere et al. (1997), Landi et al. (2006).”
EUV emission lines and diagnostics observed with Hinode/EIS (2007, methodology): “…is performing very well in terms of expected sensitivity and spectral resolution, and the observed spectra are very similar to pre-flight predictions made by Del Zanna and Mason (2005a) using the CHIANTI database (Landi et al. 2006; Dere et al. 1997) and the expected instrument parameters.”
High-precision density measurements in the solar corona I. Analysis methods and results for Fe XII and Fe XIII (2008, methodology): “Here we use version 5.2 of the CHIANTI atomic database (Landi et al. 2006; Dere et al. 1997) which contains atomic data and analysis software for calculating line ratios as a function of density.”
Models of the Solar Chromosphere and Transition Region from SUMER and HRTS Observations: Formation of the Extreme-Ultraviolet Spectrum of Hydrogen, Carbon, and Oxygen (2008, background): “The CHIANTI database, http://wwwsolar.nrl.navy.mil/chianti .html (Dere et al. 1997; Landi et al. 2006), gives the effective collision strengths for 17 of the C ii transitions we consider (2/1Y8/1, 10/1, 13/1, 3/2Y8/2, 10/2, and 13/2).”
A publicly available simulation of an enhanced network region of the Sun (2015, methodology): “Optically thin radiative losses are taken into account using tables calculated from atomic data in CHIANTI, version 5 (Dere et al. 1997; Landi et al. 2006).”
Jets in Coronal Holes: Hinode Observations and Three-dimensional Computer Modeling (2007, neutral): “2 (Landi et al. 2006) for the calculations.”
The Accretion Disk Wind in the Black Hole GRO J1655–40 (2008, methodology): “With wavelengthsfrom CHIANTI (Young et al. 2003) it is more logical to identify the line at 11.47 Å with a blue-shifted Fe XXII line at 11.51 Å.”
RHESSI Microflare Statistics. II. X-Ray Imaging, Spectroscopy, and Energy Distributions (2007, methodology): “The thermal component contains the isothermal bremsstrahlung emission (free-free and free-bound) as well as line emission from the CHIANTI database (Dere et al. 1997; Landi et al. 2006).”
CHIANTI - an atomic database for emission lines. IX. Ionization rates, recombination rates, ionization equilibria for the elements hydrogen through zinc and updated atomic data (2009, background): “The first release of CHIANTI occurred in 1996 (Dere et al. 1997) and was recently updated in 2005 (Landi et al. 2006).”
A NEW APPROACH TO ANALYZING SOLAR CORONAL SPECTRA AND UPDATED COLLISIONAL IONIZATION EQUILIBRIUM CALCULATIONS. II. UPDATED IONIZATION RATE COEFFICIENTS (2008, background): “These have been made available in a more recent CHIANTI release—version 5.2 (Landi et al. 2006).”
Deducing Electron Properties from Hard X-ray Observations (2011, methodology): “A fit to thermal bremsstrahlung alone is often adequate, but this does not account for the spectral line complexes at ∼6.7 keV and ∼8 keV or for recombination radiation.5 The thermal component of RHESSI spectra is now routinely fitted (included into standard RHESSI software) using the latest version”