Collision strengths and transition probabilities for Co iii forbidden lines

Storey, P. J.; Sochi, Taha

doi:10.1093/mnras/stw776

Cited by 10 publications

(15 citation statements)

References 26 publications

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“…νH is the hydrogen ionization rate, and νH 2 is the ionization rate of molecular hydrogen (Storey and Hummer 1995;Murray-Clay et al 2009), νH = 5.9 · 10 −8 φEUVs −1 , ν H 2 = 3.3 · 10 −8 φEUVs −1 , (A15) and ν Hcol is the collisional ionization rate (Black, 1981), ν Hcol = 5.9·10 −11 T 1/2 exp(−157809/T ) .…”

Section: Resultsmentioning

confidence: 99%

See 1 more Smart Citation

EUV-driven mass-loss of protoplanetary cores with hydrogen-dominated atmospheres: the influences of ionization and orbital distance

Еркаев¹,

Lämmer²,

Odert³

et al. 2016

Mon. Not. R. Astron. Soc.

100

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We investigate the loss rates of the hydrogen atmospheres of terrestrial planets with a range of masses and orbital distances by assuming a stellar extreme ultraviolet (EUV) luminosity that is 100 times stronger than that of the current Sun. We apply a 1D upper atmosphere radiation absorption and hydrodynamic escape model that takes into account ionization, dissociation and recombination to calculate hydrogen mass loss rates. We study the effects of the ionization, dissociation and recombination on the thermal mass loss rates of hydrogen-dominated super-Earths and compare the results to those obtained by the energy-limited escape formula which is widely used for mass loss evolution studies. Our results indicate that the energy-limited formula can to a great extent over-or underestimate the hydrogen mass loss rates by amounts that depend on the stellar EUV flux and planetary parameters such as mass, size, effective temperature, and EUV absorption radius.

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Section: Resultsmentioning

confidence: 99%

“…νH is the hydrogen ionization rate, and νH 2 is the ionization rate of molecular hydrogen (Storey and Hummer 1995;Murray-Clay et al 2009),…”

Section: Acknowledgmentsmentioning

confidence: 99%

EUV-driven mass-loss of protoplanetary cores with hydrogen-dominated atmospheres: the influences of ionization and orbital distance

Еркаев¹,

Lämmer²,

Odert³

et al. 2016

Mon. Not. R. Astron. Soc.

100

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“…Case B is a well defined limit that is a fair approximation to nebulae (AGN3 Section 4.2) and can serve as an important benchmark. Hummer & Storey (1987) and Storey & Hummer (1995) compute Case B emission and the second paper includes a series of machinereadable tables. We interpolate on these tables to include Case B predictions for H-like ions in the Cloudy output.…”

Section: Comparisons In the Case B Limitmentioning

confidence: 99%

The 2017 Release of Cloudy

Ferland,

Chatzikos,

Guzmán

et al. 2017

Preprint

211

105

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Se presenta la versión 2017 del código de síntesis espectral Cloudy junto con las mejoras de precisión y tratamiento de la física desde la version previa. La exportación de los datos atómicos hacia bases de datos externas ha permitido la incorporación de grandes conjuntos de nuevos datos. El uso completo de estos no es práctico para la mayoría de las simulaciones, describiéndose el subconjunto de datos usado por defecto y que predice un número considerable mayor de líneas que en la versión previa. No obstante, la versión actual es más rápida debido a la optimización del código. Se dan ejemplos de los límites de precisión de los modelos pequeños y de los requisitos de rendimiento para los modelos completos. Se sintetizan avances en los modelos para iones con secuencias isoelectrónicas de H y He y el uso de modelos colisionales-radiativos completos en la determinación de las densidades donde las aproximaciones coronal y de equilibrio termodinámico local funcionan.

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“…MSE Stark broadening data from [10,49,78,82,122,123] have been used in papers with the aim of determining transition probabilities in the spectra of C III [124]; N III, N IV, and N V [125]; V III [126]; Co III [127]; Cd I [128]; Cd II [128,129]; Zn II [130,131]; Au II [132,133]; Eu II and Eu III [134]; and Si IV and Ti IV [131]. Oscillator strengths have also been determined for Eu II and Eu III [134], Zn II [130,131,135], and Si IV and Ti IV [131] as well as radiative lifetimes for Cd I and Cd II [128], Au II [132], Eu II and Eu III [134], Zn II [130,131,135,136], and Si IV and Ti IV [131].…”

Section: Radiative Propertiesmentioning

confidence: 99%

Forty Years of the Applications of Stark Broadening Data Determined with the Modified Semiempirical Method

Dimitrijević

2020

Data

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The aim of this paper is to analyze the various uses of Stark broadening data for non-hydrogenic lines emitted from plasma, obtained with the modified semiempirical method formulated 40 years ago (1980), which are continuously implemented in the STARK-B database. In such a way one can identify research fields where they are applied and better see the needs of users in order to better plan future work. This is done by analysis of citations of the modified semiempirical method and the corresponding data in international scientific journals, excluding cases when they are used for comparison with other experimental or theoretical Stark broadening data or for development of the theory of Stark broadening. On the basis of our analysis, one can conclude that the principal applications of such data are in astronomy (white dwarfs, A and B stars, and opacity), investigations of laser produced plasmas, laser design and optimization and their applications in industry and technology (ablation, laser melting, deposition, plasma during electrolytic oxidation, laser micro sintering), as well as for the determination of radiative properties of various plasmas, plasma diagnostics, and investigations of regularities and systematic trends of Stark broadening parameters.

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Collision strengths and transition probabilities for Co iii forbidden lines

Cited by 10 publications

References 26 publications

EUV-driven mass-loss of protoplanetary cores with hydrogen-dominated atmospheres: the influences of ionization and orbital distance

EUV-driven mass-loss of protoplanetary cores with hydrogen-dominated atmospheres: the influences of ionization and orbital distance

The 2017 Release of Cloudy

Forty Years of the Applications of Stark Broadening Data Determined with the Modified Semiempirical Method

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