Implications of a half-millisecond pulsar
- 26 June 1989
- journal article
- research article
- Published by American Physical Society (APS) in Physical Review Letters
- Vol. 62 (26), 3015-3019
- https://doi.org/10.1103/physrevlett.62.3015
Abstract
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 1.44. The mass and baryon mass for the 1968-Hz models exceed 1.5 and 1.7, implying a progenitor mass >1.7. Those EOS’s that allowed 1968-Hz models have, for spherical stars, a stringent upper mass limit . Each model at 1968 Hz has mass above the spherical upper mass limit for its EOS, implying collapse upon spin down.
Keywords
This publication has 22 references indexed in Scilit:
- Does supernova 1987A contain a rapidly vibrating neutron star?Nature, 1989
- Low-energy Galactic-Centre γ-rays from low-mass X-ray binariesNature, 1988
- Equation of State and the Maximum Mass of Neutron StarsPhysical Review Letters, 1988
- The effect of viscosity on neutron star oscillationsThe Astrophysical Journal, 1987
- Cooling of neutron stars - Effects of the finite time scale of thermal conductionThe Astrophysical Journal, 1987
- Neutron-Star Masses as a Constraint on the Nuclear Compression ModulusPhysical Review Letters, 1986
- Estimates of the maximum angular velocity of rotating neutron starsThe Astrophysical Journal, 1986
- Implications of the millisecond pulsar for neutron star modelsThe Astrophysical Journal, 1983
- Transport properties of dense matter. IIThe Astrophysical Journal, 1979
- Generic instability of rotating relativistic starsCommunications in Mathematical Physics, 1978