THE EXCITATION OF THE PERMITTED O III NEBULAR LINES
THE EXCITATION OF THE PERMITTED O III NEBULAR LINES
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允许的 O III 星云线的激发
DOI：
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发表时间：
1934
期刊：
影响因子：
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通讯作者：
I. S. Bowen
中科院分区：
文献类型：
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作者：
I. S. Bowen
因为它们是由一个高度电离的原子发射的。P-D-P-S跃迁不在可观测范围内。然而，星云中这些线的行为仍然存在一定的差异。因此，在低激发星云中，Ne-Hi的3869和3967比O的4959和5007显得相对更强，尽管霓虹灯的所有电离阶段的电离势都比相应的氧阶段高6-8伏。还有。3342线肯定是由于与之位置重合的允许O线所致。它总是保持与线上其他O的适当强度比，并且在许多低激发星云中完全消失，在3869和3967仍然突出的星云中。Ne-Hi的p-D-p-S跃迁没有出现在星云中，这可以从一个事实中得到解释，初步计算表明，在Nein中，p-pi-p-S跃迁的可能性很大，以至于很大一部分原子通过这条路径从p S态移开。
eating that they are emitted by a very highly ionized atom. The p D — p S transition falls outside the observable range. There still remain, however, certain discrepancies in the behavior of these lines in the nebulae. Thus 3869 and 3967 of Ne hi appear relatively stronger in low-excitation nebulae than 4959 and 5007 of O in in spite of the fact that all stages of ionization of neon have ionization potentials of 6 to 8 volts higher than the corresponding stage of oxygen. Also the. 3342 line is definitely due to the permitted O in line with which it coincides in position. It always maintains the proper intensity ratio to the other O in lines as well as being completely missing in many nebulae of low excitation where 3869 and 3967 are still prominent. This failure of the p D — p S transition of Ne hi to appear in nebulae may find its explanation in the fact, suggested by a preliminary calculation, that the p Pi — p S transition is so probable in Nein that a large part of the atoms are removed from the p S state by this path.