Abstract
SOME years ago, one of us attempted to determine the kinetic temperature of atoms and a possible turbulence in some quiescent prominences1. Since at that time the different lines of a prominence had to be exposed one after the other and since only Hβ and D3 could be used for the purpose, it seemed desirable to make further observations of solar prominences with improved equipment2.
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Bruggencate, P. ten, Nachr. d. Akad. d. Wissensch. Göttingen, Math.-Phys.-Klasse, Nr. 13 (1952).
See also Unsöld, A., “Physik d. Sternatmosphären”, 2. Aufl., 682 (Springer, 1955).
Bruggencate, P. ten, and Voigt, H. H., Nachr. d. Akad. d. Wissensch. Göttingen, Math.-Phys.-Klasse, Nr. 8 (1958).
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BRUGGENCATE, P., ELSTE, G. Temperature and Turbulence in Quiescent Prominences determined from Line-widths. Nature 182, 1154 (1958). https://doi.org/10.1038/1821154a0
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DOI: https://doi.org/10.1038/1821154a0
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