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Stability Against Radial Perturbations of Slowly Rotating Neutron Stars
Published online by Cambridge University Press: 14 August 2015
Extract
The dynamical equations governing pulsation in rotating neutron stars are derived in the framework of general relativity. Stellar models are constructed by using a realistic equation of state for cold neutron matter. Small radial displacement and slow rotation are treated as perturbations on spherically symmetric body. In these models the maximum masses are 1.761 M⊙ at the central density 3.461 × 1015 g cm−3 for a sequence of nonrotating configurations and 2.165 M⊙ for rotating models with the critical angular velocity (GM/R3)½.
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- Session 7: Supernova Explosions Leading to the Formation of Neutron Stars and Black Holes
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- Copyright © Reidel 1981