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Hydrostatic equilibrium configurations of neutron stars in a non-minimal geometry-matter coupling theory of gravity

2020; Springer Science+Business Media; Volume: 80; Issue: 5 Linguagem: Inglês

10.1140/epjc/s10052-020-7958-y

ISSN

1434-6052

Autores

G. A. Carvalho, P. H. R. S. Moraes, Sérgio Ivan dos Santos, Berenice Santos Gonçalves, M. Malheiro,

Tópico(s)

Black Holes and Theoretical Physics

Resumo

In this work we analyze hydrostatic equilibrium configurations of neutron stars in a non-minimal geometry-matter coupling (GMC) theory of gravity. We begin with the derivation of the hydrostatic equilibrium equations for the $f(R,L) $ gravity theory, where $R$ and $L$ are the Ricci scalar and Lagrangian of matter, respectively. We assume $f(R,L)=R/2+[1+\sigma R]L$, with $\sigma$ constant. To describe matter inside neutron stars we assume the polytropic equation of state $p=K \rho^{\gamma}$, with $K$ and $\gamma = 5/3 $ being constants. We show that in this theory it is possible to reach the mass of massive pulsars such as PSR J2215+5135. As a feature of the GMC theory, very compact neutron stars with radius $\sim8$km and $M\sim 2.6M_\odot$ are stable, thus surpassing the Buchdal and Schwarzschild radius limits. Moreover, the referred stellar diameter is obtained within the range of observational data.

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