Tag Archives: cross sections

Improved He I Emissivities in the Case B Approximation

R.L. Porter (1), G.J. Ferland (2), P.J. Storey (3), M.J. Detisch (2) ((1)Department of Physics and Astronomy and Center for Simulational Physics, University of Georgia, Athens, GA 30602, USA;(2)Dept. of Physics & Astronomy, University of Kentucky, Lexington, KY 40506, USA; … Continue reading

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K-shell photoionization of ground-state Li-like boron ions B^{2+}: Experiment and Theory

A. Müller (1), S. Schippers (1), R. A. Phaneuf (2), S. W. J. Scully (2,3), A. Aguilar (2,4), C. Cisneros (5), M. F. Gharaibeh (2), A. S. Schlachter (4), B. M. McLaughlin (3,6) ((1)  Institut für Atom- und Molekülphysik, Justus-Liebig-Universität … Continue reading

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Valence-shell photoionization of chlorine-like Ar+ ions

A. M. Covington (1), A. Aguilar (1), I. R. Covington (1), G. Hinojosa (1), C. A. Shirley (1), R. A. Phaneuf (1), I. Álvarez (2),  C. Cisneros (2) I. Dominguez-Lopez (3), M. M. Sant’Anna (3), A. S. Schlachter (3), C. P. Ballance (4) … Continue reading

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Photoionization cross section calculations for the halogen-like ions Kr+ and Xe+

B M McLaughlin (1, 2) & C P Ballance (3) ((1) Queen’s University Belfast, Belfast, UK; (2) Harvard Smithsonian Center for Astrophysics, Cambridge, USA; (3) Auburn University, Auburn, USA) Photoionization cross sections calculations on the halogen-like ions Kr+ and Xe+ have … Continue reading

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Cross Sections for Electron Impact Excitation of O VI Lines

Haykel Elabidi (1), Sylvie Sahal-Bréchot (2), Nébil Ben Nessib (3) ((1) Groupe de Recherche en Physique Atomique et Astrophysique, Faculté des Sciences de Bizerte, Université de Carthage, Tunisia; (2) Observatoire de Paris, Meudon, France; (3) Groupe de Recherche en Physique Atomique … Continue reading

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IrOnIc: How to Consider Hundreds of Millions of Iron-Group Lines in NLTE Model-Atmosphere Calculations

Ellen Ringat (Institute for Astronomy and Astrophysics, Kepler Center for Astro and Particle Physics, Eberhard Karls University, Tuebingen, Germany) Iron-group elements have a very high number of atomic levels and an overwhelming number of spectral lines. No NLTE model-atmosphere code … Continue reading

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