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Critical angular velocity of rigidly rotating white dwarfs

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Abstract

The equilibrium configurations of rigidly rotating white dwarfs are calculated numerically as an application of the finite difference — finite expansion method pioneered by Stoeckly. The latest version of the Harrison-Wheeler equation of state is used, together with the post-Newtonian equations of structure. No other approximation is made. The resulting critical values for the angular velocity agree in order of magnitude with a ‘crude’ approximation to these values by Hartle and Thorne, but fractional differences in mean radius and in mass and eccentricities are very different.

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Authors and Affiliations

  1. Mathematics Research Center, University of Wisconsin, Madison, Wis., USA

    M. J. Miketinac

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  1. M. J. Miketinac
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On leave from Department of Applied Mathematics, University of Cape Town, Cape Town.

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Miketinac, M.J. Critical angular velocity of rigidly rotating white dwarfs. Astrophys Space Sci 44, 235–245 (1976). https://doi.org/10.1007/BF00650485

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  • DOI: https://doi.org/10.1007/BF00650485

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