2012/05/22 by Ch. C. Moustakidis, Moustakidis, Ch. C.
Earth and Planetary Sciences · Physics and Astronomy · #FOS: Physical sciences #General Relativity and Quantum Cosmology (gr-qc) #Geophysics and Gravity Measurements #High-pressure geophysics and materials #Nuclear Theory (nucl-th) #Pulsars and Gravitational Waves Research #Solar and Stellar Astrophysics (astro-ph.SR)
paper · pdf · doi:10.48550/arxiv.1205.4897
openalex publication_date 2012/05/22 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
I study the effect of nuclear equation of state on the r-mode instability of\na rotating neutron star. I consider the case where the crust of the neutron\nstar is perfectly rigid and I employ the related theory introduced by Lindblom\n it et al. citeLidblom-2000. The gravitational and the viscous time\nscales, the critical angular velocity and the critical temperature are\nevaluated by employing a phenomenological nuclear model for the neutron star\nmatter. The predicted equations of state for the \β-stable nuclear matter\nare parameterized by varying the slope L of the symmetry energy at saturation\ndensity on the interval 72.5 rm MeV \≤ L \≤ 110 rm MeV. The\neffects of the density dependence of the nuclear symmetry energy on r-mode\ninstability properties and the time evolution of the angular velocity are\npresented and analyzed. A comparison of theoretical predictions with observed\nneutron stars in low-mass x-ray binaries (LMXBs) and millisecond radio pulsars\n(MSRPs) is also performed and analyzed. I estimate that it may be possible to\nimpose constraints on the nuclear equation of state, by a suitable treatment of\nobservations and theoretical predictions of the rotational frequency and\nspindown rate evolution of known neutron stars.\n