Abstract
ANYONE who has studied the forms of the corona observed at different eclipses knows that these forms; change from time to time, going through phases which are more or less repeated every eleven or twelve years according to the soljlr activity. I have previously indicated (Monthly Notices, R.A.S., vol. Ixiii., No. 8, p. 481) that there is reason to believe that these changes of shape depend, not on sun-spot action, but on the position and percentage frequency of solar prominences, so that when prominences are most frequent, either near the solar poles or equator, the coronal streamers follow suit.
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LOCKYER, W. Prominence and Coronal Structure . Nature 77, 514–515 (1908). https://doi.org/10.1038/077514a0
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DOI: https://doi.org/10.1038/077514a0