For differentially rotating, strongly magnetized neutron stars on constant angular-momentum sequences, the normalized moment of inertia remains quasi-universal across equations of state when the Breu-Rezzolla fit is extended with magnetic and differential-rotation coefficients.
Effects of Differential Rotation on the Maximum Mass of Neutron Stars
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The merger of binary neutron stars is likely to lead to differentially rotating remnants. In this paper we numerically construct models of differentially rotating neutron stars in general relativity and determine their maximum allowed mass. We model the stars adopting a polytropic equation of state and tabulate maximum allowed masses as a function of differential rotation and stiffness of the equation of state. We also provide a crude argument that yields a qualitative estimate of the effect of stiffness and differential rotation on the maximum allowed mass.
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Structural quasi-universality in highly magnetized differentially rotating neutron stars
For differentially rotating, strongly magnetized neutron stars on constant angular-momentum sequences, the normalized moment of inertia remains quasi-universal across equations of state when the Breu-Rezzolla fit is extended with magnetic and differential-rotation coefficients.