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Stothers, R.B., 1974: Influence of rotation on the maximum mass of pulsationally stable stars. Astrophys. J., 194, 145-148, doi:10.1086/153044.
The critical mass for stability against radial pulsations in rotating, homogeneous main-sequence stars is found to be greater than in the case of no rotation. Analytic and detailed numerical models show that the critical mass rises steeply with increasing concentration of angular momentum to the center of the star. For uniform rotation near breakup velocity at the star's equator the critical mass is -850 M☉ if an electron-scattering opacity is used, or -5000 M☉ if the opacities of Cox and Stewart are used. For nonuniform rotation with a constant ratio of centrifugal force to gravity in the star, the critical mass becomes "infinite" long before breakup velocity is attained. The relevance of the present results to several observational problems is noted.
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