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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

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

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Author(s):
Carvalho, G. A. [1] ; Lobato, R. V. [1, 2, 3] ; Moraes, P. H. R. S. [1] ; Arbanil, Jose D. V. [4] ; Otoniel, E. [5] ; Marinho, Jr., R. M. [1] ; Malheiro, M. [1]
Total Authors: 7
Affiliation:
[1] Inst Tecnol Aeronaut, Dept Fis, BR-12228900 Sao Jose Dos Campos, SP - Brazil
[2] Sapienza Univ Roma, Dipartimento Fis, Ple Aldo Moro 5, I-00185 Rome - Italy
[3] ICRANet, Pzza Repubbl 10, I-65122 Pescara - Italy
[4] Univ Privada Norte, Dept Ciencias, Ave Alfredo Mendiola 6062 Urbanizac Olivos, Lima - Peru
[5] Univ Fed Cariri, Inst Formacao Prof, BR-63260000 Brejo Santo, CE - Brazil
Total Affiliations: 5
Document type: Journal article
Source: EUROPEAN PHYSICAL JOURNAL C; v. 77, n. 12 DEC 15 2017.
Web of Science Citations: 22
Abstract

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 lambda T, with lambda 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 lambda are derived. More massive and larger white dwarfs are found for negative values of lambda 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 lambda, namely, lambda > -3 x 10(-4). (AU)

FAPESP's process: 15/08476-0 - Gravitational waves in f(R,T) theories: polarization states and astrophysical sources
Grantee:Pedro Henrique Ribeiro da Silva Moraes
Support type: Scholarships in Brazil - Post-Doctorate
FAPESP's process: 13/26258-4 - Superdense matter in the universe
Grantee:Manuel Máximo Bastos Malheiro de Oliveira
Support type: Research Projects - Thematic Grants