Abstract
We provide various aspects of second rank antisymmetric Kalb–Ramond (KR) field in modified theories of gravity. The KR field energy density is found to decrease with the expansion of our universe at a faster rate in comparison to radiation and matter components. Thus as the universe evolves and cools down, the contribution of the KR field on the evolutionary process reduces significantly, and at present it almost does not affect the universe evolution. However the KR field has a significant contribution during early universe; in particular, it affects the beginning of inflation as well as increases the amount of primordial gravitational radiation and hence enlarges the value of tensor-to-scalar ratio in respect to the case when the KR field is absent. In regard to the KR field couplings, it turns out that in four dimensional higher curvature inflationary model the couplings of the KR field to other matter fields is given by 1/MPl (where MPl is known as the “reduced Planck mass” defined by MPl=18πG with G is the “Newton’s constant”) i.e., same as the usual gravity–matter coupling; however in the context of higher dimensional higher curvature model the KR couplings get an additional suppression over 1/MPl. Thus in comparison to the four dimensional model, the higher curvature braneworld scenario gives a better explanation of why the present universe carries practically no footprint of the Kalb–Ramond field. The higher curvature term in the higher dimensional gravitational action acts as a suitable stabilizing agent in the dynamical stabilization mechanism of the extra dimensional modulus field from the perspective of effective on-brane theory. Based on the evolution of KR field, one intriguing question can be—“sitting in present day universe, how do we confirm the existence of the Kalb–Ramond field which has considerably low energy density (with respect to the other components) in our present universe but has a significant impact during early universe?” We try to answer this question by the phenomena “cosmological quantum entanglement” which indeed carries the information of early universe. Finally, we briefly discuss some future perspectives of Kalb–Ramond cosmology at the end of the paper.
Highlights
Current theoretical cosmology is faced with two problems—what is inflation and what is dark energy era, or in other words, why does the universe undergo through an accelerated stage in early as well as in late time era? What is the reason that our universe behaves in a similar way at a very large and at a very low curvature scale? Apart from these problems, the initial Big-Bang singularity problem hinges the cosmological sector
Symmetry 2020, 12, 1573 spectrum [1,2,3,4,5,6,7,8,9,10,11,12,13,14,15], it does not provide any satisfactory explanation in regard to this singularity problem and the bouncing cosmology gets a lot of attention, in which case the evolution of the universe becomes free of singularity with a scale invariant perturbation spectra [16,17,18,19,20,21,22,23,24,25,26,27,28,29,30]
In the context of four dimensional higher curvature gravity theory, it turns out that the KR field energy density decreases with the expansion of our universe at a faster rate in comparison to radiation and matter components
Summary
Current theoretical cosmology is faced with two problems—what is inflation and what is dark energy era, or in other words, why does the universe undergo through an accelerated stage in early as well as in late time era? What is the reason that our universe behaves in a similar way at a very large and at a very low curvature scale? Apart from these problems, the initial Big-Bang singularity problem hinges the cosmological sector. It may be mentioned that a bulk massive scalar field or higher curvature term(s) in the bulk can generate such stable modulus potential and may act as suitable stabilizing agent in the braneworld model [87,88]. This resulted into a large volume of work on phenomenological and cosmological implications of warped geometry model [89,90,91,92,93,94,95,96,97,98,99,100,101,102,103,104,105,106].
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