CHIANTI—An Atomic Database for Emission Lines. VI. Proton Rates and Other Improvements

By Peter R. Young, G. D. Zanna, E. Landi, K. Dere, Helen E. Mason, M. Landini. 2002

258 citations recorded by the source corpus.

The CHIANTI atomic database contains atomic energy levels, wavelengths, radiative transition probabilities, and electron excitation data for a large number of ions of astrophysical interest. Version 4 has been released, and proton excitation data are now included, principally for ground configuration levels that are close in energy. The fitting procedure for excitation data, both electrons and protons, has been extended to allow nine-point spline fits in addition to the previous five-point spline fits. This allows higher quality fits to data from close-coupling calculations where resonances can lead to significant structure in the Maxwellian-averaged collision strengths. The effects of photoexcitation and stimulated emission by a blackbody radiation field in a spherical geometry on the level balance equations of the CHIANTI ions can now be studied following modifications to the CHIANTI software. With the addition of H I, He I, and N I, the first neutral species have been added to CHIANTI. Many updates to existing ion data sets are described, while several new ions have been added to the database, including Ar IV, Fe VI, and Ni XXI. The two-photon continuum is now included in the spectral synthesis routines, and a new code for calculating the relativistic free-free continuum has been added. The treatment of the free-bound continuum has also been updated.

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

View Paper: https://www.semanticscholar.org/paper/a8a04145455d7b98e45b4fbe85629943716ca5ed

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In Astronomy and Astrophysics

1. G. D. Zanna
2. M. Temmer
3. A. C. Fabian
4. S. Cranmer
5. C. Reynolds
6. Peter R. Young
7. E. Landi
8. Helen E. Mason

In Atomic and Molecular Physics, and Optics

1. G. D. Zanna
2. K. Dere
3. Peter R. Young
4. E. Landi
5. S. Cranmer
6. Helen E. Mason
7. S. Saar
8. W. Abbett

In Mechanics of Materials

1. G. D. Zanna
2. K. Dere
3. Peter R. Young
4. E. Landi
5. Helen E. Mason
6. S. Cranmer
7. W. Abbett
8. Hirohisa Hara

Citations in the corpus

• High-precision density measurements in the solar corona I. Analysis methods and results for Fe XII and Fe XIII (2008, methodology): “The method for including these latter processes in CHIANTI is described in Young et al. (2003), and examples of the effects of the processes on density diagnostics are provided in Flower & Pineau des Forêts (1973) and Young & Esser (1999a,b).”
• X-ray sources and magnetic reconnection in the X3.9 flare of 2003 November 3 (2006, methodology): “For comparison, we derived also emission measure and temperature from GOES using the up-to-date Chianti atomic model (version 4.2; Young et al. 2003) recently implemented into the GOES analysis software (White et al. 2005).”
• CHIANTI—An Atomic Database for Emission Lines. VII. New Data for X-Rays and Other Improvements (2006, methodology): “…¼ AjiW (R) !j !i k5 8 hc Uk; ð6Þ where Aji is the radiative decay rate for the transition, W(R) is the radiative dilution factor (see, e.g., Young et al. 2003), !j and !i are the statistical weights of the level j and i, respectively, h is Planck’s constant, and c is the speed of light.”
• The Magnetic Connection between the Convection Zone and Corona in the Quiet Sun (2007, methodology): “The optically thin radiative cooling curve (T ) is generated from version 4.2 of the CHIANTI atomic database (Dere et al. 1997; Young et al. 2003) as described in Lundquist et al. (2007a).”
• The EUV Imaging Spectrometer for Hinode (2007, methodology): “The response of the EIS instrument to a range of solar conditions has been calculated using synthetic spectra from the CHIANTI data base (Version 4: Dere et al., 1997; Young et al., 2003).”
• Self-consistent Coronal Heating and Solar Wind Acceleration from Anisotropic Magnetohydrodynamic Turbulence (2007, methodology): “(2) For other elements above 104 K, we used a tabulated radiative loss function from version 4.2 of the CHIANTI atomic database (Young et al. 2003) using a traditional solar abundance mixture (Grevesse & Sauval 1998) and collisional ionization balance (Mazzotta et al. 1998).”
• 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, methodology): “The merged upsilons were fit with 9 point splines (Young et al. 2003), but accurate fits could only be obtained for the reduced temperature range 3.8 ≤ log T ≤ 6.2 for which the fits are accurate to ≤1.20%.”
• An Observational Overview of Solar Flares (2011, result): “Newer continuum calculations are included in the Chianti atomic database and software package (Dere et al. 1997b; Young et al. 2003), but the dep ndence on energy and temperature is nearly the same as the earlier work.”
• CHIANTI - An atomic database for Emission Lines. Version 8 (2015, methodology): “An error in the R-matrix calculations of Zhang et al. (1994) affecting Al ix, Six, Sxii Arxiv, and Caxvi was uncovered, and corrected rates were introduced in version 4 (Young et al. 2003).”
• Ultraviolet spectroscopy of the extended solar corona (2006, methodology): “Figure 51 shows the line ratio observed at one position in the 23 April 1999 event plotted against the density dependence of the ratio predicted by CHIANTI (Young et al. 2003).”
• Dynamical and Physical Properties of a Post-Coronal Mass Ejection Current Sheet (2003, methodology): “The atomic rates are mostly adopted from the CHIANTI database version 4.01 (Dere et al. 1997; Young et al. 2003), except for the hydrogen Lyman series and [Fe xii] 1242 rates (see Ko et al. 2002 for details).”
• Updated Expressions for Determining Temperatures and Emission Measures from Goes Soft X-Ray Measurements (2005, background): “Figure 4 shows the relative contributions of free–bound, free–free and 2–photon continua for coronal and photospheric abundances at 10 MK (see also Figure 6 of Young et al., 2003, which is the same plot but for the photospheric abundance case only).”
• Double Coronal Hard and Soft X-Ray Source Observed by RHESSI: Evidence for Magnetic Reconnection and Particle Acceleration in Solar Flares (2007, methodology): “The isothermal spectrum was based on the predictions using the CHIANTI package (v. 5.2, Dere et al. 1997; Young et al. 2003) in SSW with Mazzotta et al. (1998) ionization balance.”
• Radiative Hydrodynamic Models of the Optical and Ultraviolet Emission from Solar Flares (2005, methodology): “We incorporate the effects of XEUV heating from a large number of high temperature lines using results from the CHIANTI (Dere et al. 1997; Young et al. 2003) and ATOMDB databases (Smith et al. 2001).”
• TESTING A PREDICTIVE THEORETICAL MODEL FOR THE MASS LOSS RATES OF COOL STARS (2011, methodology): “To work out its dependence onZ, we computed a number of radiative loss curves for different metal abundances using version 4.2 of the CHIANTI atomic database (Young et al. 2003) with collisional ionization balance (Mazzotta et al. 1998).”
• Solar active regions: SOHO/CDS and TRACE observations of quiescent coronal loops (2003, methodology): “The CHIANTI package (version 4.01, Young et al. 2003) has been used here to calculate the contribution functions of the observed lines, assuming collisional ionization equilibrium.”
• CHIANTI—AN ATOMIC DATABASE FOR EMISSION LINES. XII. VERSION 7 OF THE DATABASE (2012, methodology): “Proton rates for the ground transition are retained from the previous CHIANTI model (Young et al. 2003).”
• 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.”