Abstract
IN Nature of May 14, Ellison1 proposes the Stark effect in preference to the Zeeman effect as the cause of the line-broadening observed in the spectra of solar flares. However, Ellison has himself recorded2, in relation to the observed broadening of the Hα line, that “Hβ, Hγ, etc., show lesser widths, but the data are very meagre". This is the reverse of what is to be expected on the basis of the Stark effect ; but is to be expected if, as I have suggested3, the broadening is due to Zeeman effect.
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References
Ellison, M. A., Nature, 163, 749 (1949).
Ellison, M. A., and Hoyle, F., Observatory, 67, 181 (1947).
Bruce, C. E. R., Observatory (in the press).
Bruce, C. E. R., Proc. Inst. Elect. Eng., 95, Part III, 337 (1949).
Bruce, C. E. R., “A New Approach in Astrophysics and Cosmogony’ (London, 1944).
Curtiss, R. H., Pub. Ast. Observ. Univ. Michigan, 3, 1 (1923).
Wright, W. H., Lick Obs. Pub., 14, 27 (1936).
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BRUCE, C. Solar Flares and the Zeeman Effect. Nature 164, 280 (1949). https://doi.org/10.1038/164280a0
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DOI: https://doi.org/10.1038/164280a0
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