Models of rapidly rotating neutron stars

Details Models of rapidly rotating neutron stars Models of rapidly rotating neutron stars

Nov 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984natur.312..255f&link_type=abstract

Nature (ISSN 0028-0836), vol. 312, Nov. 15, 1984, p. 255-257.

Physics

39

Neutron Stars, Stellar Models, Stellar Rotation, Angular Velocity, Stellar Mass

Scientific paper

Results are reported of the first numerical construction of rapidly rotating relativistic stars based on equations of state (EOS) proposed for neutron star matter. Of nine EOS considered, none permits uniformly rotating equilibrium configurations for which the ratio of rotational energy to gravitational energy exceeds 0.12. Thus whereas a rotating neutron star spun up by accretion or formed by collapse of a rapidly rotating dwarf can be unstable to modes with a certain angular dependence for m = 3 or 4, instability to a bar mode appears very unlikely. For the stiffest EOS and for stellar masses near the Chandresekhar mass, the upper limiting rotational frequencies imposed by the m = 3 or m = 4 instability are approximately equal to the frequency of the fast pulsar; for the softer EOS, the corresponding limiting frequencies are significantly larger. Uniform rotation increases the maximum gravitational mass of a model by an amount ranging from about 14 percent for the softest models to about 30 percent for the stiffest models.

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