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Rapidly rotating neutron stars in general relativity: Realistic equations of state
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1994
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Adiabatic dissipation of energy and angular momentum drives neutron stars to evolve quasi‑stationarily along evolutionary sequences. The study aims to determine key physical parameters of rapidly rotating neutron stars, such as maximum mass and spin rate. Using a numerical scheme tailored for rapid rotation, the authors compute equilibrium sequences for 14 nuclear‑matter equations of state, assess quasi‑radial stability, and explore normal and supramassive evolutionary sequences at fixed baryon mass and entropy. The results show that supramassive sequences can exceed the nonrotating maximum mass, that such stars collapse to black holes while spinning up, and provide extensive tables of maximum masses, spin rates, and stability limits for future reference. Published in ApJ (1994), DOI 10.1086/173934, with keywords including equations of state, pulsars, relativity, and stellar evolution.
view Abstract Citations (559) References (40) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS Rapidly Rotating Neutron Stars in General Relativity: Realistic Equations of State Cook, Gregory B. ; Shapiro, Stuart L. ; Teukolsky, Saul A. Abstract We construct equilibrium sequences of rotating neutron stars in general relativity. We compare results for 14 nuclear matter equations of state. We determine a number of important physical parameters for such stars, including the maximum mass and maximum spin rate. The stability of the configurations to quasi-radial perturbations is assessed. We employ a numerical scheme particularly well suited to handle rapid rotation and large departures from spherical symmetry. We provide an extensive tabulation of models for future reference. Two classes of evolutionary sequences of fixed baryon rest mass and entropy are explored: normal sequences, which behave very much like Newtonian sequences, and supramassive sequences, which exist for neutron stars solely because of general relativistic effects. Adiabatic dissipation of energy and angular momentum causes a star to evolve in quasi-stationary fashion along an evolutionary sequence. Supramassive sequences have masses exceeding the maximum mass of a nonrotating neutron star. A supramassive star evolves toward eventual catastrophic collapse to a black hole. Prior to collapse, the star actually spins up as it loses angular momentum, an effect that may provide an observable precursor to gravitational collapse to a black hole. Publication: The Astrophysical Journal Pub Date: April 1994 DOI: 10.1086/173934 Bibcode: 1994ApJ...424..823C Keywords: Equations Of State; Pulsars; Relativity; Stellar Evolution; Stellar Models; Stellar Rotation; Angular Momentum; Black Holes (Astronomy); Computational Grids; Computerized Simulation; Equilibrium Methods; Numerical Analysis; Stability; Stellar Mass; Astrophysics; EQUATION OF STATE; STARS: PULSARS: GENERAL; RELATIVITY; STARS: NEUTRON; STARS: ROTATION full text sources ADS | data products SIMBAD (7)