Abstract
WE nave next to consider another method, which enables us to determine the motions of the solar gases. It has been already noticed that it is easy to see the prominences rushing with extreme velocity upwards in radial lines from the photosphere, and that while they are thus being carried up by some violent motion of ejection from below, they are twisted out of the radial line, now to the right, and now to the left, by what we are justified in describing as winds in the atmosphere of the sun. Those were the mere visual phenomena which were incidentally observable the moment a method was obtained of viewing the forms of prominences as well as the bright lines produced by the vapours of which they were built up, and they afforded us an opportunity of getting an insight into solar meteorology.
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LOCKYER, J. Solar Physics—the Chemistry of the Sun 1 . Nature 24, 296–301 (1881). https://doi.org/10.1038/024296a0
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DOI: https://doi.org/10.1038/024296a0