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
1988 ◽  
Vol 102 ◽  
pp. 129-132
Author(s):  
K.L. Baluja ◽  
K. Butler ◽  
J. Le Bourlot ◽  
C.J. Zeippen

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.


2013 ◽  
Author(s):  
Gillian Nave ◽  
Craig J. Sansonetti ◽  
Juliet C. Pickering ◽  
Matthew Ruffoni ◽  
Anne P. Thorne ◽  
...  

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

2019 ◽  
Vol 15 (S350) ◽  
pp. 341-344
Author(s):  
Giulio Del Zanna

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.


1988 ◽  
Vol 102 ◽  
pp. 329
Author(s):  
R.W.P. McWhirter

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.


2020 ◽  
Vol 75 (8) ◽  
pp. 739-747
Author(s):  
Feng Hu ◽  
Yan Sun ◽  
Maofei Mei

AbstractComplete and consistent atomic data, including excitation energies, lifetimes, wavelengths, hyperfine structures, Landé gJ-factors and E1, E2, M1, and M2 line strengths, oscillator strengths, transitions rates are reported for the low-lying 41 levels of Mo XXVIII, belonging to the n = 3 states (1s22s22p6)3s23p3, 3s3p4, and 3s23p23d. High-accuracy calculations have been performed as benchmarks in the request for accurate treatments of relativity, electron correlation, and quantum electrodynamic (QED) effects in multi-valence-electron systems. Comparisons are made between the present two data sets, as well as with the experimental results and the experimentally compiled energy values of the National Institute for Standards and Technology wherever available. The calculated values including core-valence correction are found to be in a good agreement with other theoretical and experimental values. The present results are accurate enough for identification and deblending of emission lines involving the n = 3 levels, and are also useful for modeling and diagnosing plasmas.


1992 ◽  
Vol 10 (3) ◽  
pp. 190-225 ◽  
Author(s):  
M. S. Atkins ◽  
M. Y. Coady

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