Abstract
MR. BRUCE believes that the short-lived broadening which we observe in the Balmer emission lines during the “flash’ phase of an intense flare arises from a temporary magnetic field of the order of 105 gauss. If this is so, some explanation is needed of the fact that no comparable Zeeman broadening has been recorded in the emission lines of iron, calcium and silicon as photographed by C. W. Allen1 and myself2. Most of these lines show (in absorption) the normal Zeeman effect in sunspot spectra, where the fields are of the order of only 103 gauss.
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References
Allen, C. W., Mon. Not. Roy. Ast. Soc., 100, 635 (1940).
Ellison, M. A., Mon. Not. Roy. Ast. Soc., 106, 500 (1946).
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ELLISON, M. Solar Flares and the Zeeman Effect. Nature 164, 280–281 (1949). https://doi.org/10.1038/164280b0
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DOI: https://doi.org/10.1038/164280b0
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