Benchmarking atomic data for astrophysics: Fe xiii EUV lines

Zanna, G. Del

doi:10.1051/0004-6361/201117121

Cited by 35 publications

(29 citation statements)

References 40 publications

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“…Vilkas & Ishikawa (2004) presented ab-initio atomic structure calculations, and suggested that in several cases misidentifications have occurred. The energies of the lower n = 3 levels have been carefully assessed in Del Zanna (2011) and are adopted here. Fig.…”

Section: Fe XIIImentioning

confidence: 99%

Benchmarking atomic data for astrophysics: a first look at the soft X-ray lines

Zanna¹

2012

A&A

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A collection of the best solar and laboratory spectra in the soft X-rays is used here to perform a preliminary benchmark in this wavelength region, by comparing observed vs. predicted wavelengths and calibrated solar irradiances. The benchmark focuses on the Fe ix -Fe xiv ions, for which we have recently calculated the relevant atomic data, however a few other ions have also been benchmarked. The iron ions are dominating the soft X-rays, however a large fraction of the strongest soft X-ray lines due to n = 4 → n = 3 transitions were previously unidentified. The strongest transitions are all identified here, in particular the decays from the core-excited levels (3s 3p l 4s, l = 5,4,3,2,1 for Fe x, Fe xi, Fe xii, Fe xiii, and Fe xiv respectively) which are the strongest soft X-ray transitions from these ions. Many new identifications are proposed, some only tentatively. Good agreement in terms of solar irradiances between the soft-Xray and EUV (n = 3 → n = 3) transitions is found, confirming the reliability of the new large-scale calculations. Some of the new atomic data and identifications are particularly important for the Solar Dynamic Observatory (SDO) Atmospheric Imaging Assembly (AIA) 94 Å band.

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Section: Fe XIIImentioning

confidence: 99%

Benchmarking atomic data for astrophysics: a first look at the soft X-ray lines

Zanna¹

2012

A&A

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“…In Table 8, the computed excitation RMCDHF/RCI energies are compared with observed energies from Del Zanna [57], as well as with energies by Vilkas and Ishikawa [58] using the MRMP method. The mean deviation is 0.076% for RMCDHF/RCI and only 0.034% for MRMP.…”

Section: Sequence Ionsmentioning

confidence: 99%

“…Comparison of calculated and observed excitation energies in cm −1 . E RCI RMCDHF/RCI energies from [56], E MRMP MRMP energies from [58] and E DZ observed energies from [57]. Relative errors in % for the calculated energies are shown in parenthesis.…”

Section: Sequence Ionsmentioning

confidence: 99%

Multiconfiguration Dirac-Hartree-Fock Calculations with Spectroscopic Accuracy: Applications to Astrophysics

Jönsson

Gaigalas

Rynkun

et al. 2017

Atoms

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Abstract:Atomic data, such as wavelengths, spectroscopic labels, broadening parameters and transition rates, are necessary for many applications, especially in plasma diagnostics, and for interpreting the spectra of distant astrophysical objects. The experiment with its limited resources is unlikely to ever be able to provide a complete dataset on any atomic system. Instead, the bulk of the data must be calculated. Based on fundamental principles and well-justified approximations, theoretical atomic physics derives and implements algorithms and computational procedures that yield the desired data. We review progress and recent developments in fully-relativistic multiconfiguration Dirac-Hartree-Fock methods and show how large-scale calculations can give transition energies of spectroscopic accuracy, i.e., with an accuracy comparable to the one obtained from observations, as well as transition rates with estimated uncertainties of a few percent for a broad range of ions. Finally, we discuss further developments and challenges.

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“…It must be mentioned that cohesiveness between atomic data producers and users has not been easy to broker in the past, in spite of periodic international conferences such as ICAMDATA [37], joint symposia (e.g., the Tenerife meeting in October 2010 on "Uncertainties in atomic data and how they propagate in chemical abundances" [38,39]), capacity development schools (e.g., NebulAtom [40]), and the AstroAtom blog [41]. However, there are exceptions to this inherent detachment, in particular the extensive astrophysical benchmarks that have been carried out of iron EUV and X-ray lines for the CHIANTI database [42][43][44][45][46][47][48][49][50][51][52][53][54][55][56]. …”

Section: Virtual Research Communitiesmentioning

confidence: 99%

AtomPy: An Open Atomic Data Curation Environment for Astrophysical Applications

Mendoza

Boswell

Ajoku

et al. 2014

Atoms

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We present a cloud-computing environment, referred to as AtomPy, based on Google-Drive Sheets and Pandas (Python Data Analysis Library) DataFrames to promote community-driven curation of atomic data for astrophysical applications, a stage beyond database development. The atomic model for each ionic species is contained in a multi-sheet workbook, tabulating representative sets of energy levels, A-values and electron impact effective collision strengths from different sources. The relevant issues that AtomPy intends to address are: (i) data quality by allowing open access to both data producers and users; (ii) comparisons of different datasets to facilitate accuracy assessments; (iii) downloading to local data structures (i.e., Pandas DataFrames) for further manipulation and analysis by prospective users; and (iv) data preservation by avoiding the discard of outdated sets. Data processing workflows are implemented by means of IPython Notebooks, and collaborative software developments are encouraged and managed within the GitHub social network. The facilities of AtomPy are illustrated with the critical assessment of the transition probabilities for ions in the hydrogen and helium isoelectronic sequences with atomic number Z ≤ 10.

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Benchmarking atomic data for astrophysics: Fe xiii EUV lines

Cited by 35 publications

References 40 publications

Benchmarking atomic data for astrophysics: a first look at the soft X-ray lines

Benchmarking atomic data for astrophysics: a first look at the soft X-ray lines

Multiconfiguration Dirac-Hartree-Fock Calculations with Spectroscopic Accuracy: Applications to Astrophysics

AtomPy: An Open Atomic Data Curation Environment for Astrophysical Applications

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