Abstract
IN a new development of the fission theory of the origin of close binary stars1,2, I showed that rotational instability would occur during the pre-main sequence contraction of rotating stars with no internal magnetic field. The theory predicted the observed mass range for contact binaries of W-Ursae Majoris type with satisfactory accuracy, and also gave the observed variation of angular momentum with mass for these systems. I now wish to show that the theory also predicts the observed relation between angular momentum and mass for all the close binary systems.
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References
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ROXBURGH, I. Angular Momenta of Eclipsing Binaries and the Fission Theory of their Origin. Nature 208, 65–66 (1965). https://doi.org/10.1038/208065b0
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DOI: https://doi.org/10.1038/208065b0
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