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2015

Stellar equilibrium configurations of compact stars in $f(R,T)$ gravity

Moraes, P. H. R. S., Arbañil, José D. V., Malheiro, M.

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In this article we study the hydrostatic equilibrium configuration of neutron stars and strange stars, whose fluid pressure is computed from the equations of state $p=\omega\rho^{5/3}$ and $p=0.28(\rho-4{\cal B})$, respectively, with $\omega$ and ${\cal B}$ being constants and $\rho$ the energy density of the fluid.

We start by deriving the hydrostatic equilibrium equation for the $f(R,T)$ theory of gravity, with $R$ and $T$ standing for the Ricci scalar and trace of the energy-momentum tensor, respectively.
Such an equation is a generalization of the one obtained from general relativity, and the latter can be retrieved for a certain limit of the theory.
For the $f(R,T)=R+2\lambda T$ functional form, with $\lambda$ being a constant, we find that some physical properties of the stars, such as pressure, energy density, mass and radius, are affected when $\lambda$ is changed.

Stellar equilibrium configurations of compact stars in $f(R,T)$ gravity · Around

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