Strange stars in energy–momentum-conserved f(R,T)f(R,T) gravity
Abstract
For the accurate understanding of compact astrophysical objects, the Tolmann–Oppenheimer–Volkoff (TOV) equation has proved to be of great use. Nowadays, it has been derived in many alternative gravity theories, yielding the prediction of different macroscopic features for such compact objects. In this work, we apply the TOV equation of the energy–momentum–conserved version of the f(R,T)f(R,T) gravity theory to strange quark stars. The f(R,T)f(R,T) theory, with f(R,T)f(R,T) being a generic function of the Ricci scalar RR and trace of the energy–momentum tensor TT to replace RR in the Einstein–Hilbert gravitational action, has shown to provide a very interesting alternative to the cosmological constant ΛΛ in a cosmological scenario, particularly in the energy–momentum conserved case (a general f(R,T)f(R,T) function does not conserve the energy–momentum tensor). Here, we impose the condition ∇μTμν=0∇μTμν=0 to the astrophysical case, particularly the hydrostatic equilibrium of strange stars. We solve the TOV equation by taking into account linear equations of state to describe matter inside strange stars, such as p=ωρp=ωρ and p=ω(ρ−4B)p=ω(ρ−4B), known as the MIT bag model, with pp the pressure and ρρ the energy density of the star, ωω constant and BB the bag constant.
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