Atomic data for astrophysics: Ni XII

G. Del Zanna, N. R. Badnell

Research output: Contribution to journalArticle

6 Citations (Scopus)

Abstract

We present new large-scale R-matrix (up to n = 4) scattering calculations for the electron collisional excitation of Cl-like Ni xii. We used the intermediate-coupling frame transformation method. We compare predicted and observed line intensities using laboratory and solar spectra, finding good agreement for all the main soft X-ray lines. With the exception of the three strongest transitions, large discrepancies with previous estimates are found, especially for the decays from the lowest 3s2 3p4 3d levels. This includes the forbidden UV lines. The atomic data for the n = 4 levels are the first to be calculated. We revise previous experimental energies, and suggest several new identifications. We point out the uncertainty in the wavelength of the 3s2 3p52P1/2-3s2 3p4 3d 2D3/2 transition, which is important for density diagnostics.

LanguageEnglish
Article numberA118
Number of pages8
JournalAstronomy and Astrophysics
Volume585
DOIs
Publication statusPublished - 6 Jan 2016

Fingerprint

astrophysics
scattering
wavelength
electron
matrix
solar spectra
energy
decay
estimates
wavelengths
excitation
electrons
x rays
laboratory
method
calculation

Keywords

  • atomic data
  • Line: identification
  • Sun: corona
  • Techniques: spectroscopic

Cite this

@article{707a2dd279ff4738b617b43e85d9b080,
title = "Atomic data for astrophysics: Ni XII",
abstract = "We present new large-scale R-matrix (up to n = 4) scattering calculations for the electron collisional excitation of Cl-like Ni xii. We used the intermediate-coupling frame transformation method. We compare predicted and observed line intensities using laboratory and solar spectra, finding good agreement for all the main soft X-ray lines. With the exception of the three strongest transitions, large discrepancies with previous estimates are found, especially for the decays from the lowest 3s2 3p4 3d levels. This includes the forbidden UV lines. The atomic data for the n = 4 levels are the first to be calculated. We revise previous experimental energies, and suggest several new identifications. We point out the uncertainty in the wavelength of the 3s2 3p52P1/2-3s2 3p4 3d 2D3/2 transition, which is important for density diagnostics.",
keywords = "atomic data, Line: identification, Sun: corona, Techniques: spectroscopic",
author = "{Del Zanna}, G. and Badnell, {N. R.}",
note = "{\circledC} ESO, 2016",
year = "2016",
month = "1",
day = "6",
doi = "10.1051/0004-6361/201527378",
language = "English",
volume = "585",
journal = "Astronomy and Astrophysics",
issn = "0004-6361",
publisher = "EDP Sciences",

}

Atomic data for astrophysics : Ni XII. / Del Zanna, G.; Badnell, N. R.

In: Astronomy and Astrophysics, Vol. 585, A118, 06.01.2016.

Research output: Contribution to journalArticle

TY - JOUR

T1 - Atomic data for astrophysics

T2 - Astronomy and Astrophysics

AU - Del Zanna, G.

AU - Badnell, N. R.

N1 - © ESO, 2016

PY - 2016/1/6

Y1 - 2016/1/6

N2 - We present new large-scale R-matrix (up to n = 4) scattering calculations for the electron collisional excitation of Cl-like Ni xii. We used the intermediate-coupling frame transformation method. We compare predicted and observed line intensities using laboratory and solar spectra, finding good agreement for all the main soft X-ray lines. With the exception of the three strongest transitions, large discrepancies with previous estimates are found, especially for the decays from the lowest 3s2 3p4 3d levels. This includes the forbidden UV lines. The atomic data for the n = 4 levels are the first to be calculated. We revise previous experimental energies, and suggest several new identifications. We point out the uncertainty in the wavelength of the 3s2 3p52P1/2-3s2 3p4 3d 2D3/2 transition, which is important for density diagnostics.

AB - We present new large-scale R-matrix (up to n = 4) scattering calculations for the electron collisional excitation of Cl-like Ni xii. We used the intermediate-coupling frame transformation method. We compare predicted and observed line intensities using laboratory and solar spectra, finding good agreement for all the main soft X-ray lines. With the exception of the three strongest transitions, large discrepancies with previous estimates are found, especially for the decays from the lowest 3s2 3p4 3d levels. This includes the forbidden UV lines. The atomic data for the n = 4 levels are the first to be calculated. We revise previous experimental energies, and suggest several new identifications. We point out the uncertainty in the wavelength of the 3s2 3p52P1/2-3s2 3p4 3d 2D3/2 transition, which is important for density diagnostics.

KW - atomic data

KW - Line: identification

KW - Sun: corona

KW - Techniques: spectroscopic

UR - http://www.scopus.com/inward/record.url?scp=84954286545&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201527378

DO - 10.1051/0004-6361/201527378

M3 - Article

VL - 585

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

SN - 0004-6361

M1 - A118

ER -