The most important integral characteristics of the rotating white dwarfs and super dense configurations are calculated with the approximation linear to the parameter characterizing the rotation beta. It is shown that the angular velocities of the rotation of neutron stars may appreciably exceed that to the white dwarfs. The rotation in a small region to the central densities, corresponding to the maximum value of the mass breaks the stable equilibrium of white dwarfs. In the corresponding region, the neutron stars are much more stable in relation to the rotation. In the region of metastable neutron stars, the rotation occurs to be the perturbation which breaks the equilibrium of the matter.
Communications of the Byurakan Astrophysical Observatory
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