Constraining $f(T,B)$ teleparallel gravity from energy conditions

Snehasish Bhattacharjee

doi:10.1016/j.newast.2020.101495

paper

Constraining $f (T, B)$ teleparallel gravity from energy conditions

arXiv:2004.12060 · doi:10.1016/j.newast.2020.101495

Abstract

$f (T, B)$ teleparallel gravity is a recently proposed straightforward generalization of the popular $f (T)$ teleparallel gravity by the incorporation of a boundary term $B = \frac{2}{e} \partial_{i} (e T^{i}) = ▽_{i} T^{i}$ where $T$ denote the torsion scalar \cite{ftb13}. In this work, I investigate the viability of some well motivated $f (T, B)$ teleparallel gravity models of the forms $f = α B^{n} + β T^{m}$ , $f = α B^{n} T^{m}$ and $f = α lo g (B) + β T$ where $α, β, n$ and $m$ are free parameters from the inequalities imposed the the weak energy condition. I use the recent estimates of Hubble, deceleration, jerk and snap parameters in finding corners in parameter spaces for the cosmological models for which the energy density remain positive and the weak energy condition ( i.e, $ρ + p \geq 0$ , where $p$ and $ρ$ represent respectively the cosmological pressure and energy density) attains a minute positive value, as this implies the EoS parameter $ω = p / ρ ≃ - 1$ and therefore consistent with an accelerating universe.

Accepted in New Astronomy

Constraining $f (T, B)$ teleparallel gravity from energy conditions

Abstract

References in corpus (13)

Cited by in corpus (9)

Constraining f(T,B) teleparallel gravity from energy conditions

Abstract

References in corpus (13)

Cited by in corpus (9)

Constraining $f (T, B)$ teleparallel gravity from energy conditions