A potential-based method constructs stationary, differentially rotating, non-barotropic neutron stars in general relativity, with dynamical evolutions supporting that they are equilibrium configurations.
Spin evolution of a proto-neutron star
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abstract
We study the evolution of the rotation rate of a proto-neutron star, born in a core-collapse supernova, in the first seconds of its life. During this phase, the star evolution can be described as a sequence of stationary configurations, which we determine by solving the neutrino transport and the stellar structure equations in general relativity. We include in our model the angular momentum loss due to neutrino emission. We find that the requirement of a rotation rate not exceeding the mass-shedding limit at the beginning of the evolution implies a strict bound on the rotation rate at later times. Moreover, assuming that the proto-neutron star is born with a finite ellipticity, we determine the emitted gravitational wave signal, and estimate its detectability by present and future ground-based interferometric detectors.
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Rotating neutron stars with non-barotropic thermal profile
A potential-based method constructs stationary, differentially rotating, non-barotropic neutron stars in general relativity, with dynamical evolutions supporting that they are equilibrium configurations.