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Neutron stars in $f(R,T)$ gravity with conserved energy-momentum tensor: Hydrostatic equilibrium and asteroseismology

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arxiv 2105.07573 v2 pith:4FLPJCIW submitted 2021-05-17 gr-qc astro-ph.HE

Juan M. Z. Pretel , Sergio E. Jorás , Ribamar R. R. Reis , José D. V. Arbañil This is my paper
classification gr-qcastro-ph.HE
keywords bindingenergyenergy-momentumgravitytensorcuspequationequations
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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.

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Cited by 2 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Rotating Fermion-Boson Stars in $R$-squared Gravity

    gr-qc 2026-07 conditional novelty 6.0 of 10

    R-squared gravity enlarges the equilibrium domain of rotating fermion-boson stars and raises static and Keplerian maximum masses relative to GR while remaining compatible with current compact-object constraints.

  2. Mass-Gap Neutron Stars from Vector \texorpdfstring{$f(R)$}{f(R)} Gravity Inflationary Deformations

    gr-qc 2025-07 conditional novelty 4.0 of 10

    Using four vector f(R) gravity inflation models and nine equations of state, the TOV solver finds that the MPA1 equation of state yields neutron star maximum masses around 2.75 solar masses, inside the mass gap.

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