Limiting rotational period of neutron stars
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 lowdensity equation of state, uncertainties in which can be evaluated as to their effect on the result. This establishes a limiting curve in the massperiod 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 {ital M}=1.442{ital M}{sub {circle dot}} 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 selfbound in bulk at a sufficiently large equilibrium energy density, can lie in the region above the generalrelativistic forbidden region, and in the region forbidden to neutron stars.
 Authors:

^{[1]}
 (Nuclear Science Division, Lawrence Berkeley Laboratory, University of California, Berkeley, California 94720 (United States))
 Publication Date:
 OSTI Identifier:
 6950413
 DOE Contract Number:
 AC0376SF00098
 Resource Type:
 Journal Article
 Resource Relation:
 Journal Name: Physical Review, D (Particles Fields); (United States); Journal Volume: 46:10
 Country of Publication:
 United States
 Language:
 English
 Subject:
 72 PHYSICS OF ELEMENTARY PARTICLES AND FIELDS; NEUTRON STARS; ROTATION; BLACK HOLES; CAUSALITY; EINSTEIN FIELD EQUATIONS; ENERGY DENSITY; EQUATIONS OF STATE; GENERAL RELATIVITY THEORY; GRAVITATIONAL INTERACTIONS; MASS; QUARK MATTER; WAVE EQUATIONS; BASIC INTERACTIONS; DIFFERENTIAL EQUATIONS; EQUATIONS; FIELD EQUATIONS; FIELD THEORIES; INTERACTIONS; MATTER; MOTION; PARTIAL DIFFERENTIAL EQUATIONS; STARS 662110*  General Theory of Particles & Fields Theory of Fields & Strings (1992)