Fig. 1.

The radius R of a uniformly rotating star increases sharply as the Kepler (mass-shedding) limit ($\mathit{\Omega }={\mathit{\Omega }}_K$) is approached. The particular sequence of models shown here has a constant central energy density of ${\mathit{ϵ}}_c=1.21\times {10}^{15}{\mathrm{g}\mathrm{cm}}^{-3}$ and was constructed with EOS L. (Image reproduced with permission from Stergioulas and Friedman 1995, copyright by AAS)