Tag Archives: NLTE

The diagnostic potential of Fe lines applied to protostellar jets

Posted on May 20, 2014 by

Giannini, T. (1); Nisini, B. (1); Antoniucci, S. (1); Alcalá, J. M. (2); Bacciotti, F. (3); Bonito, R. (4,5); Podio, L. (6); Stelzer, B. (4); Whelan, E. T. (7) (1) INAF-Osservatorio Astronomico di Roma, via Frascati 33, I-00040 Monte Porzio Catone, Italy; (2) INAF-Osservatorio Astronomico di Capodimonte, via Moiariello 16, I-80131 … Continue reading →

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Strontium: To LTE or non-LTE that is the question

Posted on December 31, 2012 by

C. J. Hansen (1), M. Bergemann (2), G. Cescutti (3), P. Francois (4), A. Arcones (5), A. I. Karakas (6), K. Lind (2), and C. Chiappini (3) ((1) Landessternwarte, ZAH, K ̈ nigstuhl 12, 69117 Heidelberg, Germany; (2) Max-Planck Institute … Continue reading →

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Astrophysical tests of atomic data important for stellar Mg abundance determinations

Posted on December 22, 2012 by

L. Mashonkina (1,2) ((1) Universitäts-Sternwarte München, Scheinerstr. 1, D-81679 München, Germany; (2) Institute of Astronomy, Russian Academy of Sciences, RU-119017 Moscow, Russia) Magnesium abundances of cool stars with different metallicities are important for understanding the galactic chemical evolution. This study … Continue reading →

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NLTE line formation of Fe for late-type stars. I. Standard stars with 1D and model atmospheres

Posted on November 27, 2012 by

Maria Bergemann (1), K. Lind (1), R. Collet (2,3,1), Z. Magic (1) and M. Asplund (4,1) ((1)Max Planck Institute for Astrophysics, Karl-Schwarzschild Str. 1, 85741, Garching, Germany; (2) Natural History Museum of Denmark, Centre for Star and Planet Formation, Øster … Continue reading →

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NLTE analysis of Sr lines

Posted on November 12, 2012 by

Bergemann, M. (1), Hansen, C. J. (2) Bautista, M. (3) and Ruchti, G. (4) ((1) Max-Planck Institute for Astrophysics, Karl-Schwarzschild Str. 1, 85741, Garching, Germany; (2) Landessternwarte, Königstuhl 12, 69117, Heidelberg, Germany; (3) Department of Physics, Western Michigan University, Kalamazoo, … Continue reading →

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NLTE analysis of Sr lines in spectra of late-type stars with new R-matrix atomic data

Posted on August 27, 2012 by

M. Bergemann (1), C. J. Hansen (2), M. Bautista (3), and G. Ruchti (1) ((1) Max-Planck Institute for Astrophysics, Karl-Schwarzschild Str. 1, 85741, Garching, Germany; (2) Landessternwarte, K¨onigstuhl 12, 69117 Heidelberg, Germany; (3) Department of Physics, Western Michigan University, Kalamazoo, … Continue reading →

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The Carina Project. V. The impact of NLTE effects on the iron content

Posted on April 25, 2012 by

M. Fabrizio (1), T. Merle (2), F. Thévenin (2), M. Nonino (4), G. Bono (1,4), P. B. Stetson (5,6), I. Ferraro (4), G. Iannicola (4), M. Monelli (7,8), A. R. Walker (9), R. Buonanno (1,10), F. Caputo (4), C. E. … Continue reading →

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NLTE determination of the calcium abundance and 3D corrections in extremely metal-poor stars

Posted on April 7, 2012 by

M. Spite (1), S.M. Andrievsky (1,2), F. Spite1, E. Caffau (3,1), S.A. Korotin (2), P. Bonifacio (1), H.-G. Ludwig (3), P. François (1), and R. Cayrel (1) ((1) GEPI Observatoire de Paris, CNRS, Universite Paris Diderot,Meudon Cedex, France; (2) Department … Continue reading →

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Lithium in M67: from the main sequence to the red giant branch

Posted on March 21, 2012 by

Giancarlo Pace (1), Matthieu Castro (2), Jorge Meléndez (3), Sylvie Théado(4) & José-Dias do Nascimento Jr. (2) ((1) Centro de Astrofísica, Universidade do Porto, Rua das Estrelas, Porto, Portugal; (2) Departamento de Física Teórica e Experimental, Universidade Federal do Rio Grande do Norte, RN, Brazil; (3) Departamento de Astronomia do IAG/USP, Universidade de … Continue reading →

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Non-LTE effects on the lead and thorium abundance determinations for cool stars

Posted on February 14, 2012 by

L. Mashonkina (1, 2),  A. Ryabtsev (3) and A. Frebel (4,5) ((1) Universitäts-Sternwarte München, Scheinerstr, München, Germany; (2) Russian Academy of Sciences, RU, Moscow, Russia; (3) Russian Academy of Sciences, 142190, Troitsk, Moscow region, Russia; (4) Kavli Institute for Astrophysics … Continue reading →

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