Atomic data for iron-group elements of astrophysical interest

2013 ◽  
Author(s):  
Gillian Nave ◽  
Craig J. Sansonetti ◽  
Juliet C. Pickering ◽  
Matthew Ruffoni ◽  
Anne P. Thorne ◽  
...  
Keyword(s):  
Atomic Data ◽  
Iron Group ◽  
Astrophysical Interest

Recent Radiative and Collisional Atomic Data of Astrophysical Interest

1988 ◽  
Vol 102 ◽  
pp. 129-132
Author(s):  
K.L. Baluja ◽  
K. Butler ◽  
J. Le Bourlot ◽  
C.J. Zeippen
Keyword(s):  
Mass Production ◽  
Bound States ◽  
Physical Models ◽  
Impact Excitation ◽  
Electron Impact Excitation ◽  
Atomic Data ◽  
Isoelectronic Sequence ◽  
Astrophysical Interest ◽  
Radiative Transitions ◽  
Forbidden Transitions

SummaryUsing sophisticated computer programs and elaborate physical models, accurate radiative and collisional atomic data of astrophysical interest have been or are being calculated. The cases treated include radiative transitions between bound states in the 2p4and 2s2p5configurations of many ions in the oxygen isoelectronic sequence, the photoionisation of the ground state of neutral iron, the electron impact excitation of the fine-structure forbidden transitions within the 3p3ground configuration of CℓIII, Ar IV and K V, and the mass-production of radiative data for ions in the oxygen and fluorine isoelectronic sequences, as part of the international Opacity Project.

RECENT RADIATIVE AND COLLISIONAL ATOMIC DATA OF ASTROPHYSICAL INTEREST

1988 ◽  
Vol 49 (C1) ◽  
pp. C1-129-C1-132 ◽  
Author(s):  
K. L. BALUJA ◽  
K. BUTLER ◽  
J. LE BOURLOT ◽  
C. J. ZEIPPEN
Keyword(s):  
Atomic Data ◽  
Astrophysical Interest

scholarly journals New laboratory atomic data for neutral, singly, and doubly ionised iron group elements for astrophysics applications

2015 ◽  
Vol 11 (A29A) ◽  
Author(s):  
Juliet C. Pickering ◽  
Gillian Nave ◽  
Florence Liggins ◽  
Christian Clear ◽  
Matthew Ruffoni ◽  
...  
Keyword(s):  
Group Element ◽  
Atomic Data ◽  
Iron Group

AbstractWe report new measurements of atomic data for the neutral, singly and doubly ionised iron group element spectra for modern astrophysics applications.

scholarly journals Line-blanketing in massive stars: new results

1999 ◽  
Vol 193 ◽  
pp. 129-137
Author(s):  
D. John Hillier
Keyword(s):  
Massive Stars ◽  
Emission Lines ◽  
Atomic Data ◽  
Iron Group ◽  
Numerical Techniques ◽  
Hot Stars ◽  
Charge Exchange Reaction ◽  
Present Generation ◽  
Individual Line

Until recently, a major deficiency of most spectroscopic modeling of hot stars was the neglect of line-blanketing. With the availability of new atomic data, faster computers, suitable approximations, and improved numerical techniques it is now feasible to include non-LTE line-blanketing due to CNO and iron group elements in atmospheric calculations. We highlight the capabilities of the present generation of models. New blanketing results are presented for WN and WC Wolf-Rayet stars, and for LBVs. Line-blanketing alters individual line strengths in unpredictable ways, and can significantly influence the determination of stellar parameters. We specifically highlight the UV spectral region in which the effects of Fe blanketing are directly manifested. The importance of the charge exchange reaction Fe2+ + H ⇌ Fe+ + H+ for modeling of the Fe emission lines in the extreme P-Cygni star HDE 316285 is illustrated.

scholarly journals Atomic data for VUV lines of astrophysical interest in singly ionized rhodium

2011 ◽  
Vol 184 (3-6) ◽  
pp. 174-176 ◽  
Author(s):  
P. Quinet ◽  
É. Biémont ◽  
P. Palmeri ◽  
L. Engström ◽  
H. Hartman ◽  
...  
Keyword(s):  
Atomic Data ◽  
Astrophysical Interest

scholarly journals Comprehensive atomic wavelengths, energy levels, and hyperfine structure for singly ionized iron-group elements

2017 ◽  
Vol 95 (9) ◽  
pp. 811-816 ◽  
Author(s):  
Gillian Nave ◽  
Craig J. Sansonetti ◽  
Keeley Townley-Smith ◽  
Juliet C. Pickering ◽  
Anne P. Thorne ◽  
...  
Keyword(s):  
Hyperfine Structure ◽  
Recent Work ◽  
Energy Levels ◽  
Imperial College ◽  
Iron Group ◽  
Astrophysical Interest

We summarize recent work at the National Institute of Standards and Technology and Imperial College London on wavelengths, hyperfine structure, energy levels, and analysis of singly ionized iron-group elements of astrophysical interest.

Benchmarked atomic data for astrophysics

2019 ◽  
Vol 15 (S350) ◽  
pp. 341-344
Author(s):  
Giulio Del Zanna
Keyword(s):  
High Resolution ◽  
Spectral Line ◽  
Extreme Ultraviolet ◽  
Stellar Atmospheres ◽  
Atomic Data ◽  
X Rays ◽  
Astrophysical Interest ◽  
X Ray ◽  
Line Intensities

AbstractThe recent calculations of atomic data for ions of astrophysical interest are reviewed with a focus on work performed in Cambridge. The calculations have been benchmarked against high-resolution laboratory and astrophysical spectra. A framework for assessing uncertainties in atomic data has also been developed. Long-standing discrepancies in predicted spectral line intensities have been resolved, and a significant number of levels in coronal ions have finally been identified, improving the modelling of the extreme-ultraviolet and soft X-ray spectral regions. Recent improvements based on collisional-radiative modelling are presented. They are relevant for the modelling of satellite lines in the X-rays and for solving the long-standing problems in the chromosphere-corona transition in stellar atmospheres.

The Interpretation of Solar Spectral Intensities

1988 ◽  
Vol 102 ◽  
pp. 329
Author(s):  
R.W.P. McWhirter
Keyword(s):  
Emission Measure ◽  
Physical Nature ◽  
Atomic Data ◽  
The Sun ◽  
Atomic Properties ◽  
Outer Atmosphere ◽  
Spectral Intensities ◽  
Thin Plasma ◽  
Number Of Authors

The intensity of a specrtal line from an optically thin plasma such as the outer atmosphere of the sun depends on both the atomic properties of the atomic ion responsible for the line and the physical nature of the plasma. In this paper we discuss the various ways in which the measured spectral intensities from the sun are used to discover something about the nature of the sun’s atmosphere. The technique has been referred to as the emission measure method. It has important limitations in terms of the accuracy of the specrtal data as well as the atomic data. We discuss some of these and suggest methods by which they may be assessed. The technique is illustrated by application to real observations from a number of authors.

Electrodeposition of Strained-Layer Superlattices

1996 ◽  
Vol 451 ◽  
Author(s):  
T. P. Moffat
Keyword(s):  
Charge Transfer ◽  
Mass Transport ◽  
Structural Evolution ◽  
Iron Group ◽  
Morphological Instability ◽  
Group Metal ◽  
Iron Group Metal ◽  
Transport Control ◽  
Strained Layer Superlattices ◽  
Interfacial Charge

ABSTRACTA variety of Cu/(Ni, Co) multilayers have been grown on Cu single crystals by pulse plating from an alloy electroplating bath. Copper is deposited under mass transport control while the iron group metal is deposited under interfacial charge transfer control. The structural evolution of these films is influenced by the morphological instability of the mass transport limited copper deposition reaction and the development of growth twins during iron-group metal deposition. Specular films have been obtained for growth on Cu(100) while rough, defective films were typically obtained for growth on Cu(111) and Cu(110).

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