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From the intensities of the green nebular lines the density of 0 iii ions proves to be roughly i per cm3, corresponding to an abundance about ten thousand times less than that of the hydrogen ions. The numbers, nevertheless, are sufficient to produce a marked depression of the electron temperature, through the medium of coffisional excitation. The observed electron temperatures, given in Paper XIII, are con- sistent with the theory developed in Paper V, modified for the effects of collisions
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Menzel et al. (1941) studied this question.
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