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

Carvalho, G. A. ; Lobato, R. V. ; Moraes, P. H. R. S. ; Arbañil, José D. V. ; Otoniel, E. ; Marinho, R. M. ; Malheiro, M.

The European physical journal. C, Particles and fields, 2017-12, Vol.77 (12), p.1-8, Article 871 [Periódico revisado por pares]

Berlin/Heidelberg: Springer Berlin Heidelberg

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Título:
Stellar equilibrium configurations of white dwarfs in the f(R, T) gravity
Autor: Carvalho, G. A. ; Lobato, R. V. ; Moraes, P. H. R. S. ; Arbañil, José D. V. ; Otoniel, E. ; Marinho, R. M. ; Malheiro, M.
Assuntos: Astronomy ; Astrophysics and Cosmology ; Configurations ; Elementary Particles ; Equilibrium ; Equilibrium equations ; Flux density ; Gravitation ; Gravity ; Hadrons ; Heavy Ions ; Measurement Science and Instrumentation ; Nuclear Energy ; Nuclear Physics ; Physical properties ; Physics ; Physics and Astronomy ; Quantum Field Theories ; Quantum Field Theory ; Regular Article - Theoretical Physics ; String Theory ; White dwarf stars
É parte de: The European physical journal. C, Particles and fields, 2017-12, Vol.77 (12), p.1-8, Article 871
Descrição: 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 λ T , 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 .
Editor: Berlin/Heidelberg: Springer Berlin Heidelberg
Idioma: Inglês

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

Carvalho, G. A. ; Lobato, R. V. ; Moraes, P. H. R. S. ; Arbañil, José D. V. ; Otoniel, E. ; Marinho, R. M. ; Malheiro, M.

Berlin/Heidelberg: Springer Berlin Heidelberg

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