The solar coronal X-ray spectrum from 15.4 to 23.0 A - Lines from highly ionized calcium and chromium and their usefulness as plasma diagnostics

McKenzie, D. L.; Landecker, P. B.

doi:10.1086/159735

Cited by 21 publications

(10 citation statements)

References 10 publications

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“…The N -like spectra do not give rise to very strong lines, and for this reason Nitrogen like minor elements lines have seldom been observed. We find some relatively weak lines of the lighter minor elements in the spectra of SERTS (Thomas & Neupert 1994), SUMER , while some lines from Cr XVIII have been observed around 15Å by McKenzie & Landecker (1982), which also point out the importance of chromium as plasma diagnostic for hot plasmas.…”

Section: Nitrogen Isoelectronic Sequencesupporting

confidence: 54%

“…The Fluorine-like minor ions give rise to very weak lines and therefore to our knowledge there are no direct observations of their lines in astrophysical plasmas, with the only exception of Cr XVI (Acton 1985;McKenzie & Landecker 1982). F-like minor ions lines are potentially detectable by the CDS spectrometer from Na III to P VII.…”

Section: Fluorine Isoelectronic Sequencementioning

confidence: 89%

“…Only some lines of the highly ionized Cr XVII have been observed by McKenzie & Landecker (1982). Nevertheless lines for the lighter ions of the sequence are observable by the CDS spectrometer on board on SOHO and some identifications of these lines are suggested by Brooks et al (1998).…”

Section: Oxygen Isoelectronic Sequencementioning

confidence: 95%

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The Arcetri spectral code for thin plasmas

Landi

Landini

1998

Astron. Astrophys. Suppl. Ser.

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Abstract. The Arcetri spectral code allows to evaluate the spectrum of the radiation emitted by hot and optically thin plasmas in the spectral range 1 − 2000Å. The database has been updated including atomic data and radiative and collisional rates to calculate level population and line emissivities for a number of ions of the minor elements; a critical compilation of the electron collision excitation for these elements has been performed. The present version of the program includes the CHIANTI database for the most abundant elements, the minor elements data, and Fe III atomic model, radiative and collisional data.

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Section: Nitrogen Isoelectronic Sequencesupporting

confidence: 54%

Section: Fluorine Isoelectronic Sequencementioning

confidence: 89%

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The Arcetri spectral code for thin plasmas

Landi

Landini

1998

Astron. Astrophys. Suppl. Ser.

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“…Ca xvii Landi & Bhatia (2009a) provide the Ca xvii data set that we use here. They also reviewed the experimental energies available for this ion from Edlén (1983Edlén ( , 1985, Hayes (1975), andLandecker (1982). Experimental energies, used for CHIANTI 6, were available only for the n = 2, 3 levels and none were available for the n = 4, 5 levels.…”

Section: Ar XVmentioning

confidence: 99%

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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“…It was Ðrst identiÐed as the photospheric Fe La characteristic line, arising from innershell ionization by coronal X-rays (McKenzie et al 1980 ;Phillips et al 1982). However, this has subsequently been questioned on the grounds that the observed line is both stronger than expected and that its observed wavelength and width do not quite correspond to that of Fe La (McKenzie & Landecker 1982 ;Acton et al 1985). Two other candidate identiÐcations have been advanced : a second order Fe XXIII line at 8.815 (Fawcett et al 1987) A and an Fe XVIII line predicted in a theoretical investigation of the Fe XVIII spectrum (Cornille et al 1992).…”

Section: Introductionmentioning

confidence: 99%

On Photospheric Fluorescence and the Nature of the 17.62 A Feature in Solar X‐Ray Spectra

Drake

Swartz

Beiersdörfer

et al. 1999

ApJ

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The identiÐcation of the emission-line feature at 17.62 in solar X-ray spectra is reexamined. Using a A Monte Carlo technique, we compute a realistic theoretical upper limit to the observed Fe La photospheric Ñuorescent line strength caused by irradiation from an overlying corona. These calculations demonstrate that the photospheric Fe La characteristic line is much too weak to account for the observed 17.62line Ñux. Instead, we identify this line with the conÐguration interaction 2s22p43p A transition in Fe XVIII seen in Electron Beam Ion Trap spectra and predicted in earlier 2P 3@2 È2s2p6 2S 1@2 theoretical work on the Fe XVIII X-ray spectrum. This line should be easily resolved and detected in stellar coronae by the spectrographs on the upcoming Chandra X-ray Observatory and X-ray Multimirror Mission.

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The solar coronal X-ray spectrum from 15.4 to 23.0 A - Lines from highly ionized calcium and chromium and their usefulness as plasma diagnostics

Cited by 21 publications

References 10 publications

The Arcetri spectral code for thin plasmas

The Arcetri spectral code for thin plasmas

CHIANTI – an atomic database for emission lines

On Photospheric Fluorescence and the Nature of the 17.62 A Feature in Solar X‐Ray Spectra

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