Equilibrium models of axisymmetric, zero-temperature stars in differential rotation, representing possible final states of stellar evolution, are presented in detafl for the mass range 1 3-4 1 Mo. Total angular momenta of the computed models are in agreement with those estimated from observations of main-sequence stars of the corresponding masses Physical effects which limit the range of validity of the models, including viscosity and the occurrence of dynamical instabilities, are briefly discussed
No takes yet. Share an insight, caveat, or question.
Ostriker et al. (1968) studied this question.