The Stability of the Atmosphere of a Rotating Star

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Abstract
It is shown that electromagnetic forces acting on the gaseous ions of a rotating magnetized star can account for its atmospheric stability even when the star proper approaches a condition of rotational instability. Milne's theory of the chromospheric stability is shown to be inconsistent with observation if electromagnetic forces are taken into account. Because the ions are entrapped by the magnetic field the loss of atmosphere by a rapidly rotating star is small and therefore its angular velocity may increase until rotational instability of the entire mass sets in. The considerations of the paper lend considerable theoretical support to the fission theory of multiple stars.