Implications of a half-millisecond pulsar

Details Implications of a half-millisecond pulsar Implications of a half-millisecond pulsar

Jun 1989

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1989phrvl..62.3015f&link_type=abstract

Physical Review Letters (ISSN 0031-9007), vol. 62, June 26, 1989, p. 3015-3019.

Physics

109

Neutron Stars, Pulsars, Stellar Models, Equations Of State, Stellar Mass, Stellar Rotation

Scientific paper

New models of rotating neutron stars show that only a surprisingly narrow range of possible equations of state (EOSs) can simultaneously allow a rotating neutron star with frequency as large as 1968 Hz and a spherical (nonrotating) neutron star with mass as large as 1.44 solar mass. The mass and baryon mass for the 1968-Hz models exceed 1.5 solar mass and 1.7 solar mass, implying a progenitor mass larger than 1.7 solar mass. Those EOSs that allowed 1968-Hz models have, for spherical stars, a stringent upper mass limit of 1.7 solar mass. Each model at 1968 Hz has mass above the spherical upper mass limit for its EOS, implying collapse upon spin down.

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