Inflation with F(T) teleparallel gravity

Abstract

We study early universe with a particular form of F(T) teleparallel gravity theory, in which inflation is driven by a scalar field. To ensure slow rollover, two different potentials are chosen in a manner, such that they remain almost flat for large initial value of the scalar field. Inflationary parameters show wonderful fit with the presently available Planck's data set. The energy scale of inflation is sub-Planckian, and graceful exit from inflation is also administered. The chosen form of F(T) administers late-time cosmic acceleration too. In the process, unification of the early inflation with late-time acceleration is ensured. Unfortunately, a decelerated radiation-dominated era is only possible with a different form of (quartic) potential, which being devoid of a flat section does not admit slow rollover.

Dynamics and Stability via Thin‐Shell of Approximated Black Holes in f(Q)$f(\mathbb {Q})$ Gravity

“…As a result, the Lanczos equations may be used for symmetric teleparallel gravity as they serve as a link between the two theories and a tool for exploring and comprehending gravity dynamics in this setting. [83,84] Researchers can make use of the well-established knowledge and resources created in the area of general relativity and apply them to examine the characteristics and behavior of gravity in symmetric teleparallel gravity by employing the Lanczos equations. The Lanczos equations are used in symmetric teleparallel gravity, which not only broadens their range of applications but also makes it easier to contrast and link the two theories.…”

Reconstructing Modified and Alternative Theories of Gravity

“…On the contrary, it may be mentioned that different forms of F(R) emerge in different eras, in view of Noether symmetry [11].…”

The issue of Branched Hamiltonian in F(T) Teleparallel Gravity

“…although, it is not a new one. In fact, plugging in p 2 a from (11), one can retrieve T + 6 ȧ2 a 2 = 0 . Next, since {ξ, χ} = 0 , so the constraint is second class as mentioned, and one has to make the consistency check by finding,…”

“…Regarding the above form of F (T ) we recall that the form F (T ) = (T 2 + 6βT − 3β 2 )) [7] and F (T ) = T + T 2 − c [16] are outcome of reconstruction program, which is the simplest generalization of F (T ) gravity. Further, the form F (T ) = αT + βT 2 has already been treated by several authors [11,17,18], particularly to study early inflation and late stage of cosmic acceleration. In this section, we therefore proceed to construct the Hamiltonian in view of this form of F (T ).…”

“…As already mentioned, F (T ) gravity has been introduced to drive late-stage of cosmic acceleration without the need for dark energy. A scalar field (φ) has therefore been introduced in the above action (8) to drive inflation at the very early stage of cosmic evolution [11]. Now varying the action with respect to T one gets λ = F ′ (T ), where F ′ (T ) is the derivative of F (T ) with respect to T .…”