Energy Levels of Iron, Fe I Through Fe XXVI

Reader, Joseph; Sugar, Jack

doi:10.1063/1.555659

Cited by 195 publications

(74 citation statements)

References 18 publications

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“…These have been determined by optimizing the sum of the energies of all the 262 LS-coupling terms from all the configurations. The main difference between the target used here and that of BZ is the number of levels so that there is little difference in the quality of the agreement with the observed energy level data of Corliss & Sugar (1982). This is shown in Table 3 where only those levels with observed values are to be found.…”

Section: Methodsmentioning

confidence: 86%

Atomic data from the IRON project

Butler¹,

Badnell²

2008

A&A

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Context. Accurate electron collisional data are required for the analysis of the Fe xix astrophysical spectrum, in particular in the sun.Such an analysis can provide information on the physical characteristics of the coronal plasma.Aims. An extensive target is used in an R-matrix scattering calculation to provide the necessary data for Fe 18+ . The use of the R-matrix method includes the resonance contribution lacking in the distorted wave approach and the large target improves the accuracy of the close-coupling approximation. Methods. The R-Matrix package described by Berrington et al. (1995, Comput. Phys. Commun., 92, 290) as provided by the UK RmaX project has been used to calculate electron collisional data among 342 levels of Fe

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Section: Methodsmentioning

confidence: 86%

Atomic data from the IRON project

Butler¹,

Badnell²

2008

A&A

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“…Unlike SNe IIn, the iron lines seen in SN 2010da do not arise from continual shock heating over hundreds of days. Instead, these lines arise in regions of diffuse gas surrounding the progeny, which are heated to temperatures of about 2×10 6 K, the approximate ionization temperature for lines such as [Fe XII] and [Fe XIV] (Corliss & Sugar 1982), by X-rays from the compact companion (see Section 4.3).…”

Section: Fe Linesmentioning

confidence: 99%

The Intermediate Luminosity Optical Transient Sn 2010da: The Progenitor, Eruption, and Aftermath of a Peculiar Supergiant High-Mass X-Ray Binary

Villar

Berger

Chornock

et al. 2016

ApJ

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We present optical spectroscopy, ultraviolet-to-infrared imaging,and X-ray observations of the intermediate luminosity optical transient (ILOT) SN 2010da in NGC 300 (d = 1.86 Mpc) spanning from −6 to +6 years relative to the time of outburst in 2010. Based on the light-curve and multi-epoch spectral energy distributions of SN 2010da, we conclude that the progenitor of SN 2010da is a ≈10-12 M e yellow supergiant possibly transitioning into a blue-loop phase. During outburst, SN 2010da had a peak absolute magnitude of M bol −10.4 mag, dimmer than other ILOTs and supernova impostors. We detect multi-component hydrogen Balmer, Paschen, and Ca II emission lines in our high-resolution spectra, which indicate a dusty and complex circumstellar environment. Since the 2010 eruption, the star has brightened by a factor of ≈5 and remains highly variable in the optical. Furthermore, we detect SN 2010da in archival Swift and Chandra observations as an ultraluminous X-ray source (L X ≈ 6 × 10 39 erg s −1). We additionally attribute He II 4686 Å and coronal Fe emission lines in addition to a steady X-ray luminosity of ≈10 37 erg s −1 to the presence of a compact companion.

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“…For Ne vii n = 3 energy levels the data of Tondello & Paget (1970) were supplemented by the data of Bashkin & Stoner (1975). For Si xi, Ar xv and Ti xix the energies given by Fawcett (1984Fawcett ( , 1985 were adopted, while for Fe xxiii the results of Corliss & Sugar (1982) supplemented by data from Fawcett (1984Fawcett ( , 1985 were used. For the transition probabilities for 2-3 transitions from 2s 2 and 2s 2p levels to levels 3 the data of Fawcett (1984Fawcett ( , 1985 were chosen and for transitions from 2p 2 levels to n = 3 levels the results of Sampson et al (1984) were used.…”

Section: Be-like Ionsmentioning

confidence: 99%

“…Energy levels were taken from Jupén et al (1993) and Corliss & Sugar (1982). Oscillator strengths were from a 24 configuration model Superstructure calculation for the CHIANTI database.…”

Section: Fe Ionsmentioning

confidence: 99%

ADAS analysis of the differential emission measure structure of the inner solar corona

Lanzafame

Brooks

Lang

et al. 2002

A&A

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Abstract. The differential emission measure (DEM) of a solar active region is derived from SERTS-89 rocket data between 170 and 450Å . The integral inversion to infer the DEM distribution from spectral line intensities is performed by the data adaptive smoothing approach (Thompson 1990(Thompson , 1991. Our analysis takes into account the density dependence of both ionisation fractions and excitation coefficients according to the collisional-radiative theory as implemented in ADAS, the Atomic Data and Analysis Structure (McWhirter & Summers 1984;Summers 1994;Summers 2001). Our strategy aims at checking, using observational data, the validity and limitations of the DEM method used for analysing solar EUV spectra. We investigate what information it is possible to extract, within defined limitations, and how the method can assist in a number of cases, e.g. abundance determination, spectral line identification, intensity predictions, and validation of atomic cross-sections. Using the above data and theory, it is shown that a spurious multiple peak in the DEM distribution between log(Te) = 6.1 and 6.7, where Te is the electron temperature, may derive from an inaccurate treatment of the population densities of the excited levels and ionisation fractions or from using an integral inversion technique with arbitrary smoothing. Therefore, complex DEM structures, like those proposed for solar and stellar coronae by several authors, must be considered with caution. We address also the issue of systematic differences between iso-electronic sequences and show that these cannot be unambiguously detected in the coronal lines observed by SERTS. Our results indicate that a substantial improvement is required in the atomic modelling of the complex element Fe. The elemental abundance ratio Si/Ne is found to be close to its photospheric value. The same result may be true for the Fe/Ne abundance, but this latter result is uncertain because of the problems found with Fe.

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Energy Levels of Iron, Fe I Through Fe XXVI

Cited by 195 publications

References 18 publications

Atomic data from the IRON project

Atomic data from the IRON project

The Intermediate Luminosity Optical Transient Sn 2010da: The Progenitor, Eruption, and Aftermath of a Peculiar Supergiant High-Mass X-Ray Binary

ADAS analysis of the differential emission measure structure of the inner solar corona

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