2021/05/31 by Juan M. Z. Pretel, Sergio E. Jorás, Sérgio E. Jorás +2 · 1 citation
Physics and Astronomy · #Asteroseismology #Astrophysics #Black Holes and Theoretical Physics #Chandrasekhar limit #Classical mechanics #Cosmology and Gravitation Theories #Equation of state #Exact solutions in general relativity #Hydrostatic equilibrium #Mathematical physics #Neutron star #Physics #Polytropic process #Pulsars and Gravitational Waves Research #Quantum electrodynamics #Quantum mechanics #Stars #Stress–energy tensor #Tensor (intrinsic definition) #White dwarf #astro-ph.HE #gr-qc
paper · pdf · doi:10.1088/1475-7516/2021/08/055
published as JCAP 08 (2021) 055 · 21 pages, 8 figures
openalex publication_date 2021/08/01 · arxiv created 2021/08/25 · arxiv updated 2021/08/26 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/06
Abstract We investigate the equilibrium and radial stability of spherically symmetric relativistic stars, considering a polytropic equation of state (EoS), within the framework of f(R,T) gravity with a conservative energy-momentum tensor. Both modified stellar structure equations and Chandrasekhar's pulsation equations are derived for the f(R,T)= R+ h(T) gravity model, where the function h(T) assumes a specific form in order to safeguard the conservation equation for the energy-momentum tensor. The neutron star properties, such as radius, mass, binding energy and oscillation spectrum are studied in detail. Our results show that a cusp — which signals the appearance of instability — is formed when the binding energy is plotted as a function of the compact star proper mass. We find that the squared frequency of the fundamental vibration mode passes through zero at the central-density value corresponding to such a cusp where the binding energy is a minimum.