Astronomy and Astrophysics – Astrophysics
Scientist
Astronomy and Astrophysics
Astrophysics
Scientist
Faculty of Physics, University of Belgrade, P.O. Box 368, Studentski Trg 14, 11001 Belgrade, Serbia and Montenegro.
Beograd, Univerzitet, Belgrade, Yugoslavia
Faculty of Physics, University of Belgrade, 11001 Belgrade, PO Box 368, Serbia; Isaac Newton Institute of Chile, Yugoslavia Branch, Belgrade, Serbia
Faculty of Physics, University of Belgrade, 11 001 Belgrade, PO Box 368, Serbia
Faculty of Physics, University of Belgrade PO Box 368, 11000 Belgrade, Serbia, Yugoslavia
Faculty of Physics, University of Belgrade, Studentski trg 12-16, P.O.Box 368, 11000 Belgrade, Serbia
Belgrade, University, Yugoslavia
Faculty of Physics, University of Belgrade, 11001 Belgrade, PO Box 368, Serbia, Yugoslavia; Isaac Newton Institute of Chile, Yugoslavia Branch, Belgrade, Yugoslavia; Hungarian Academy of Sciences, Budapest, Hungary
Beograd, Universitet, Belgrade, Yugoslavia
Faculty of Physics, University of Belgrade, 11001 Belgrade, PO 368, Serbia ; Isaac Newton Institute of Chile, Yugoslavia Branch, Belgrade, Serbia
Faculty of Physics, University of Belgrade, PO Box 368, Belgrade, Serbia, Yugoslavia; Hungarian Academy of Science, Budapest, Hungary
Faculty of Physics, University of Belgrade, P.O. Box 368, Serbia, Belgrade, Yugoslavia
Faculty of Physics, University of Belgrade, P.O. Box 368, 11001 Belgrade, Serbia, Yugoslavia
Faculty of Physics
Faculty of Physics, University of Belgrade, PO Box 368, Belgrade, Serbia
Faculty of Physics, University of Belgrade, Studentski trg 12-16, P.O. Box 368, 11 000 Belgrade, Serbia of Physics, University of Belgrade, POB 368, Belgrade, Serbia; Isaac Newton Institute of Chile, Yugoslavia Branch, Belgrade, Serbia; Hungarian Academy of Sciences, Budapest, Hungary
Faculty of Physics, University of Belgrade, P.O. Box 368 Belgrade, Serbia, Yugoslavia
Faculty of Physics, University of Belgrade, PO Box 368, Belgrade, Serbia; Isaac Newton Institute of Chile, Yugoslavia Branch, Bel
Astrophysical plasma diagnostics through analysis of Ar I line shape characteristics
Bowen Fluorescence, Stark Broadening, and Transition Probabilities in the O III Spectrum
Contribution of ion to the astrophysical important 471.32 nm He I spectral line broadening
Experimental and calculated Stark widths within the Kr I spectrum
Experimental Stark shift of several N II and O II spectral lines.
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