NUMERICAL-SOLUTIONS OF GENERAL-RELATIVISTIC FIELD-EQUATIONS FOR RAPIDLY ROTATING NEUTRON-STARS

Stationary axial symmetric equilibrium configurations rapidly rotating with uniform angular velocity in the framework of general relativity are considered. Sequences of models are numerically computed by means of a computer code that solves the full Einstein equations exactly. Th is code employs Neugebauer's minimal surface formalism, where the fiel d equations are equivalent to two-dimensional minimal surface equation s for 4 metric potentials. The calculations are based upon 10 differen t equations of state. Results of various structures of neutron stars a nd the rotational effects on stellar structures and properties are rep orted. Finally some limits to equations of state of neutron stars and the stability for rapidly rotating relativistic neutron stars are disc ussed.