Spin evolution of a proto-neutron star

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.

10 pages, 5 figures; minor changes to match the version published on Phys.Rev.D

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Cited by in corpus (11)

• Approximate Universal Relations for Neutron Stars and Quark Stars
• A new temperature dependent hyperonic equation of state: application to rotating neutron star models and I-Q-relations
• General relativistic models for rotating magnetized neutron stars in conformally flat spacetime
• EoS for hot neutron stars
• Rotating neutron stars with non-barotropic thermal profile
• Continuous gravitational waves from Galactic neutron stars: demography, detectability and prospects
• Axisymmetric models for neutron star merger remnants with realistic thermal and rotational profiles
• Asymmetric core collapse of rapidly rotating massive star
• Exotic Baryons in Hot Neutron Stars
• Evolution of proto-neutron stars to pulsars, magnetars and central compact objects
• Asymmetric emissions of neutrinos in the cooling of rotating proto-neutron stars