TY - JOUR

T1 - Stellar equilibrium configurations of white dwarfs in the f(R, T) gravity

AU - Carvalho, G. A.

AU - Lobato, R. V.

AU - Moraes, P. H.R.S.

AU - Arbañil, José D.V.

AU - Otoniel, E.

AU - Marinho, R. M.

AU - Malheiro, M.

N1 - Publisher Copyright:
© 2017, The Author(s).

PY - 2017/12/1

Y1 - 2017/12/1

N2 - In this work we investigate the equilibrium configurations of white dwarfs in a modified gravity theory, namely, f(R, T) gravity, for which R and T stand for the Ricci scalar and trace of the energy-momentum tensor, respectively. Considering the functional form f(R, T) = R+ 2 λT, with λ being a constant, we obtain the hydrostatic equilibrium equation for the theory. Some physical properties of white dwarfs, such as: mass, radius, pressure and energy density, as well as their dependence on the parameter λ are derived. More massive and larger white dwarfs are found for negative values of λ when it decreases. The equilibrium configurations predict a maximum mass limit for white dwarfs slightly above the Chandrasekhar limit, with larger radii and lower central densities when compared to standard gravity outcomes. The most important effect of f(R, T) theory for massive white dwarfs is the increase of the radius in comparison with GR and also f(R) results. By comparing our results with some observational data of massive white dwarfs we also find a lower limit for λ, namely, λ> - 3 × 10 - 4.

AB - In this work we investigate the equilibrium configurations of white dwarfs in a modified gravity theory, namely, f(R, T) gravity, for which R and T stand for the Ricci scalar and trace of the energy-momentum tensor, respectively. Considering the functional form f(R, T) = R+ 2 λT, with λ being a constant, we obtain the hydrostatic equilibrium equation for the theory. Some physical properties of white dwarfs, such as: mass, radius, pressure and energy density, as well as their dependence on the parameter λ are derived. More massive and larger white dwarfs are found for negative values of λ when it decreases. The equilibrium configurations predict a maximum mass limit for white dwarfs slightly above the Chandrasekhar limit, with larger radii and lower central densities when compared to standard gravity outcomes. The most important effect of f(R, T) theory for massive white dwarfs is the increase of the radius in comparison with GR and also f(R) results. By comparing our results with some observational data of massive white dwarfs we also find a lower limit for λ, namely, λ> - 3 × 10 - 4.

UR - http://www.scopus.com/inward/record.url?scp=85038353496&partnerID=8YFLogxK

U2 - 10.1140/epjc/s10052-017-5413-5

DO - 10.1140/epjc/s10052-017-5413-5

M3 - Artículo

AN - SCOPUS:85038353496

SN - 1434-6044

VL - 77

JO - European Physical Journal C

JF - European Physical Journal C

IS - 12

M1 - 871

ER -