Limiting rotational period of neutron stars

Details Limiting rotational period of neutron stars Limiting rotational period of neutron stars

Nov 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992phrvd..46.4161g&link_type=abstract

Physical Review D (Particles, Fields, Gravitation, and Cosmology), Volume 46, Issue 10, 15 November 1992, pp.4161-4168

Physics

35

Neutron Stars, Relativity And Gravitation, Stellar Rotation

Scientific paper

We seek an absolute limit on the rotational period for a neutron star as a function of its mass, based on the minimal constraints imposed by Einstein's theory of relativity, Le Chatelier's principle, causality, and a low-density equation of state, uncertainties in which can be evaluated as to their effect on the result. This establishes a limiting curve in the mass-period plane below which no pulsar that is a neutron star can lie. For example, the minimum possible Kepler period, which is an absolute limit on rotation below which mass shedding would occur, is 0.33 ms for a M=1.442Msolar neutron star (the mass of PSR1913+16). A still lower curve, based only on the structure of Einstein's equations, limits any star whatsoever to lie in the plane above it. Hypothetical stars such as strange stars, if the matter of which they are made is self-bound in bulk at a sufficiently large equilibrium energy density, can lie in the region above the general-relativistic forbidden region, and in the region forbidden to neutron stars.

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