IONIZATION BALANCE FOR OPTICALLY THIN PLASMAS: RATE COEFFICIENTS FOR Cu, Zn, Ga, and Ge IONS

Mazzitelli, G.; Mattioli, M.

doi:10.1006/adnd.2002.0887

Cited by 19 publications

(26 citation statements)

References 44 publications

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“…Further interpolations were performed by Landini & Monsignori Fossi (1990) and Landini & Monsignori Fossi (1991) for F, Al, P, Cl, K, Ti, Cr, Mn, and Co and these values are also included here. The rate coefficients for Cu and Zn were obtained from Mazzitelli & Mattioli (2002). The radiative recombination rate coefficients for Sc and V have been interpolated here.…”

Section: Radiative Recombinationmentioning

confidence: 99%

“…For the ions of Sc and V, we have used the rates of Mazzotta et al (1998) but, as noted above, it is not always clear how these rates were determined. The rate coefficients for Cu and Zn were obtained from Mazzitelli & Mattioli (2002).…”

Section: Al Through Ar Isoelectronic Sequencesmentioning

confidence: 99%

“…They are available for Ca ii (Jacobs et al 1980), Fe ii , Fe iii (Nahar 1997), Fe iv (Nahar 1996), Fe v (Nahar et al 1998), Fe vi (Nahar & Bautista 1999) and Ni iii Nahar & Bautista (2001). In addition, the rate coefficients of Mazzitelli & Mattioli (2002) are available for Cu and Zn. Many rates rely on the Burgess general formula (GF) (Burgess 1965) but it is not clear how accurately it can be applied to these complex ions.…”

Section: K Through Mn Isoelectronic Sequencesmentioning

confidence: 99%

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CHIANTI – an atomic database for emission lines

Dere¹,

Landi²,

Young³

et al. 2009

A&A

464

451

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Aims. The goal of the CHIANTI atomic database is to provide a set of atomic data for the interpretation of astrophysical spectra emitted by collisionally dominated, high temperature, optically thin sources. Methods. A complete set of ground level ionization and recombination rate coefficients has been assembled for all atoms and ions of the elements of H through Zn and inserted into the latest version of the CHIANTI database, CHIANTI 6. Ionization rate coefficients are taken from the recent work of Dere (2007, A&A, 466, 771) and recombination rates from a variety of sources in the literature. These new rate coefficients have allowed the calculation of a new set of ionization equilibria and radiative loss rate coefficients.For some ions, such as Fe viii and Fe ix, there are significant differences from previous calculations. In addition, existing atomic parameters have been revised and new atomic parameters inserted into the database. Results. For each ion in the CHIANTI database, elemental abundances, ionization potentials, atomic energy levels, radiative rates, electron and proton collisional rate coefficients, ionization and recombination rate coefficients, and collisional ionization equilibrium populations are provided. In addition, parameters for the calculation of the continuum due to bremsstrahlung, radiative recombination and two-photon decay are provided. A suite of programs written in the Interactive Data Language (IDL) are available to calculate line and continuum emissivities and other properties. All data and programs are freely available at http://wwwsolar.nrl.navy.mil/ chianti

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Section: Radiative Recombinationmentioning

confidence: 99%

Section: Al Through Ar Isoelectronic Sequencesmentioning

confidence: 99%

Section: K Through Mn Isoelectronic Sequencesmentioning

confidence: 99%

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CHIANTI – an atomic database for emission lines

Dere¹,

Landi²,

Young³

et al. 2009

A&A

464

451

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“…[25] for Fe and Ni and from Ref. [26] for Ge, the F-like to B-like charge states could not be simulated unless the relevant α rec /S ion ratios were increased. In another paper on M-shell Ni spectra in the 144-180 Å region [23] both D(r) and V(r) were known from similar discharges and with best fits on the strongest lines of the involved Ni X-XV ions, the best sets of data for both ionisation and recombination have been obtained.…”

Section: Spectral Analysis Of Impuritiesmentioning

confidence: 99%

“…At present, the most recent article in this context is the 1998 paper from Mazzotta et al [25], which has been extended in Ref. [26] from Cu to Ge (Z=32). Assessments and updates of these atomic data have been started both by us and at the Columbia University under the leadership of D. Savin [27].…”

Section: Figurementioning

confidence: 99%

Spectral Line Shapes as a Diagnostic Tool in Magnetic Fusion

Stamm¹,

Capes²,

Demura³

et al. 2006

AIP Conference Proceedings

Self Cite

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Abstract. Spectral line shapes and intensities are used for obtaining information on the various regions of magnetic fusion devices. Emission from low principal quantum numbers of hydrogen isotopes is analyzed for understanding the complex recycling mechanism. Lines emitted from high principal quantum numbers of hydrogen and helium are dominated by Stark effect, allowing an electronic density diagnostic in the divertor. Intensities of lines emitted by impurities are fitted for a better knowledge of ion transport in the confined plasma.

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Ionisation Equilibrium for the Non-Maxwellian Electron n $n$ -Distributions in Solar Flares: Updated Calculations

Dzifčáková¹,

Dudík²

2016

Solar and Stellar Flares

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IONIZATION BALANCE FOR OPTICALLY THIN PLASMAS: RATE COEFFICIENTS FOR Cu, Zn, Ga, and Ge IONS

Cited by 19 publications

References 44 publications

CHIANTI – an atomic database for emission lines

CHIANTI – an atomic database for emission lines

Spectral Line Shapes as a Diagnostic Tool in Magnetic Fusion

Ionisation Equilibrium for the Non-Maxwellian Electron n $n$ -Distributions in Solar Flares: Updated Calculations

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