Phase Transitions in Rotating Neutron Stars

Abstract

As rotating neutron stars slow down, the pressure and the density in the core region increase due to the decreasing centrifugal forces and phase transitions may occur in the center. We extract the analytic behavior near the critical angular velocity ${\Omega }_0$, where the phase transitions occur in the center of a neutron star, and calculate the moment of inertia, angular velocity, rate of slow down, braking index, etc. For a first order phase transition these quantities have a characteristic behavior, e.g., the braking index diverges as $\sim ({\Omega }_0-\Omega {)}^{-1/2}$. Observational consequences for first, second and other phase transitions are discussed.

5 pages, one figure included, revtex latex style

References in corpus (2)

• Spin-Isospin Structure and Pion Condensation in Nucleon Matter
• Signal of Quark Deconfinement in the Timing Structure of Pulsar Spin-Down

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