1998/01/30 by Bithin Datta, B. Datta, Arun V. Thampan +6
Earth and Planetary Sciences · Physics and Astronomy · #Astro and Planetary Science #Astrophysics (astro-ph) #FOS: Physical sciences #Geophysics and Gravity Measurements #Pulsars and Gravitational Waves Research #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/9801312
Accepted for publication in main journal of Astronomy and Astrophysics. Replaced with a new version of manuscript (previous submission was a wrong version and did not contain all figures). 6 pages manuscript with 5 tables and 8 figures separate
openalex publication_date 1998/01/30 · arxiv created 1998/02/17 · arxiv updated 2016/08/14 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
For four newly suggested microscopic equations of state of neutron star matter, we construct equilibrium sequences of rapidly rotating neutron stars in general relativity. The sequences are the normal and supramassive evolutionary sequences of constant rest mass. We find that for these equations of state the maximum (gravitational) mass rotating models occur (in central density and rotation rate Ω) before the maximum--Ω models. We calculate equilibrium sequences for a constant value of Ω corresponding to the most rapidly rotating pulsar PSR 1937+21. Also calculated is the radius of the marginally stable orbit and its dependence on Ω.