CHIANTI - an atomic database for emission lines. IX. Ionization rates, recombination rates, ionization equilibria for the elements hydrogen through zinc and updated atomic data

By K. Dere, E. Landi, Peter R. Young, G. D. Zanna, M. Landini, Helen E. Mason. 2009

394 citations recorded by the source corpus.

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

View Paper: https://www.semanticscholar.org/paper/6f4646bfda1e6921cd753b6631cf25c0800e53fd

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. G. D. Zanna
2. Peter R. Young
3. E. Landi
4. K. Dere
5. Helen E. Mason
6. C. Schrijver
7. R. Sutherland
8. A. Title

In Atomic and Molecular Physics, and Optics

1. G. D. Zanna
2. Peter R. Young
3. K. Dere
4. E. Landi
5. Helen E. Mason
6. R. Sutherland
7. I. Hannah
8. A. Foster

In Mechanics of Materials

1. G. D. Zanna
2. Peter R. Young
3. K. Dere
4. E. Landi
5. Helen E. Mason
6. R. Sutherland
7. I. Hannah
8. Randall K. Smith

Citations in the corpus

• GLOBAL ENERGETICS OF THIRTY-EIGHT LARGE SOLAR ERUPTIVE EVENTS (2012, methodology): “…loss rate vs. temperature function (for coronal abundances and Mazzotta et al. (1998) ionization equilibria) taken from the CHIANTI database (Dere et al. 1997, 2009), we used the IDL procedure rad loss, available in SSW, to calculate, for each 3-s time interval, the energy radiated from the…”
• How much H and He is ‘hidden’ in SNe Ib/c? – I. Low-mass objects (2012, background): “Rate coefficients for the - mal collisional excitation to or between levels withn > 4, however, have conveniently been taken from the rate compilations CHIANTI (Dere et al. 1997, 2009) and TMAD (Rauch & Deetjen 2003).”
• A SYSTEMATIC SURVEY OF HIGH-TEMPERATURE EMISSION IN SOLAR ACTIVE REGIONS (2012, methodology): “…and the emission measure distribution by the usual expression Iλ = 1 4π ∫ ǫλ(ne, Te)ξ(Te) dTe, (1) whereǫλ(ne, Te) is the emissivity computed with the CHIANTI atomic database version 7 assuming coronal abundances (Feldman et al. 1992) and the CHIANTI ionization fractions (Dere et al. 2009).”
• CHIANTI - An atomic database for Emission Lines. Version 8 (2015, methodology): “The effect of cascades following recombination into He-like levels of C V, N VI, O VII, Ne IX, Mg XI and Si XIII was modeled by Porquet & Dubau (2000), and these data were added to CHIANTI v.6 (Dere et al. 2009).”
• LYα TRANSIT SPECTROSCOPY AND THE NEUTRAL HYDROGEN TAIL OF THE HOT NEPTUNE GJ 436b (2014, methodology): “Instead we use their C II emission line variability, because C II has a similar formation temperature to Lyman-α (Tform ≈ (1 − 3) × 104 K, Dere et al. 2009).”
• Differential Emission Measures from the Regularized Inversion of Hinode and SDO data (2012, methodology): “To test the regularization with more physically realistic DEMs we use those provided with the CHIANTI atomic database (Dere et al. 1997, 2009).”
• SDO/AIA response to coronal hole, quiet Sun, active region, and flare plasma (2010, methodology): “For this purpose we have used CHIANTI v. 6.0.1 (Dere et al. 1997, 2009) atomic data and ionization equilibrium.”
• CHIANTI—An Atomic Database for Emission Lines. XV. Version 9, Improvements for the X-Ray Satellite Lines (2019, methodology): “The effective collision strengths for the bound levels were not correctly extrapolated above 7 MK when they were processed for CHIANTI 6 (Dere et al. 2009), and so the data have been re-processed for CHIANTI 9.”
• CHIANTI—AN ATOMIC DATABASE FOR EMISSION LINES. XII. VERSION 7 OF THE DATABASE (2012, background): “Since the latest release (Dere et al. 2009), many new atomic physics calculations were published that improved the data sets for several ions in CHIANTI, or provided new data for transitions unavailable in the literature before.”
• The Atmospheric Imaging Assembly (AIA) on the Solar Dynamics Observatory (SDO) (2011, methodology): “Responses to solar emissions are computed assuming the CHIANTI solar spectral model (Dere et al., 1997, 2009).”
• UPDATED ATOMIC DATA AND CALCULATIONS FOR X-RAY SPECTROSCOPY (2012, background): “0.1 data (Dere et al. 2009), which was the current version at the time of preparation of this data set.”
• The multi-thermal emission in solar active regions (2013, background): “A notable feature is a change in the ionization equilibrium for Feviii and Feix, compared to the previous one (Dere et al. 2009).”