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Title: Limiting rotational period of neutron stars

Abstract

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 {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 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.

Authors:
 [1]
  1. (Nuclear Science Division, Lawrence Berkeley Laboratory, University of California, Berkeley, California 94720 (United States))
Publication Date:
OSTI Identifier:
6950413
DOE Contract Number:
AC03-76SF00098
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-)

Citation Formats

Glendenning, N.K. Limiting rotational period of neutron stars. United States: N. p., 1992. Web. doi:10.1103/PhysRevD.46.4161.
Glendenning, N.K. Limiting rotational period of neutron stars. United States. doi:10.1103/PhysRevD.46.4161.
Glendenning, N.K. 1992. "Limiting rotational period of neutron stars". United States. doi:10.1103/PhysRevD.46.4161.
@article{osti_6950413,
title = {Limiting rotational period of neutron stars},
author = {Glendenning, N.K.},
abstractNote = {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 {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 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.},
doi = {10.1103/PhysRevD.46.4161},
journal = {Physical Review, D (Particles Fields); (United States)},
number = ,
volume = 46:10,
place = {United States},
year = 1992,
month =
}
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