Phys. Rev. Lett. 62, 3015–3019 (1989)Implications of a half-millisecond pulsarReceived 15 March 1989; published in the issue dated 26 June 1989 New models of rotating neutron stars show that only a surprisingly narrow range of possible equations of state (EOS’s) 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 1.44M⊙. The mass and baryon mass for the 1968-Hz models exceed 1.5M⊙ and 1.7M⊙, implying a progenitor mass >1.7M⊙. Those EOS’s that allowed 1968-Hz models have, for spherical stars, a stringent upper mass limit <1.7M⊙. Each model at 1968 Hz has mass above the spherical upper mass limit for its EOS, implying collapse upon spin down. © 1989 The American Physical Society URL:
http://link.aps.org/doi/10.1103/PhysRevLett.62.3015
DOI:
10.1103/PhysRevLett.62.3015
PACS:
97.60.Jd, 21.65.+f, 97.60.Gb
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