Full text  
Author(s): 
Total Authors: 3

Affiliation:  ^{[1]} Inst Tecnol Aeronaut, Dept Fis, BR12228900 Sao Paulo  Brazil
Total Affiliations: 1

Document type:  Journal article 
Source:  Journal of Cosmology and Astroparticle Physics; n. 6 JUN 2016. 
Web of Science Citations:  48 
Abstract  
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  4B), respectively, with omega and beta 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 energymomentum 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. We show that for a fixed central star energy density, the mass of neutron and strange stars can increase with lambda. Concerning the star radius, it increases for neutron stars and it decreases for strange stars with the increment of lambda. Thus, in f (R, T) theory of gravity we can push the maximum mass above the observational limits. This implies that the equation of state cannot be eliminated if the maximum mass within General Relativity lies below the limit given by observed pulsars. (AU)  
FAPESP's process:  15/084760  Gravitational waves in f(R,T) theories: polarization states and astrophysical sources 
Grantee:  Pedro Henrique Ribeiro da Silva Moraes 
Support type:  Scholarships in Brazil  PostDoctorate 