Abstract
We derive a limit on the rotation period of a gravitationally bound star that is analogous to Ruffini's mass limit for a neutron star. We discuss the impact of gravitational radiation-reaction instabilities. The condition that self-bound stars can rotate faster is derived. The present status of searches for fast pulsars is reviewed. The composition of neutron stars is discussed in the context of nuclear and hypernuclear constraints. The phase transition from hadron to quark phase in the interior of dense neutron stars is discussed properly accounting for the fact that this first order phase transition involves two conserved charges. Hybrid stars are then described.
Published Version
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