Abstract
We extend the Induced Matter Theory of gravity (IMT) to 5D curved spacetimes by using the Weitzenböck representation of connections on a 5D curved spacetime. In this representation the 5D curvature tensor becomes null, so that we can make a static foliation on the extra non-compact coordinate to induce in the Weitzenböck representation the Einstein equations. Once we have done it, we can rewrite the effective 4D Einstein equations in the Levi-Civita representation. This generalization of IMT opens a huge window of possible applications for this theory. A pre-big bang collapsing scenario is explored as an example.
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Notes
In our conventions indices “a,b,c,…,h” run from 1 to 5, “A,B,C,…,H” run from 1 to 5, Greek indices α,β,γ run from 1 to 4 and indices “i,j,k,…” run from 2 to 4.
Notice that for fermionic fields (for instance with spin 1/2), the Cartan equation (22) should be
$$ \overbrace{{S}_{\beta\gamma}}^{\mathrm{4D}} - \frac{1}{2} \sigma_{\beta\gamma} S =-8 \pi G \,\underbrace{\overbrace {{T}_{\beta\gamma}}^{\mathrm{4D}}}_{(\mathrm{ant})}, $$where S=σ μν S μν , \(\sigma^{\mu\nu}={1\over2} [\gamma^{\mu}, \gamma^{\nu} ]\) and γ μ are the Dirac matrices. However, this issue is beyond the scope of this work.
In the cases where \(M_{\mathrm{eff}}^{2} >0\) and the universe expands with a nearly constant energy density given by ρ≃〈V(φ)〉 and a pressure P≃−〈V(φ)〉, the potential (55) is a good candidate to describe inflation.
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Acknowledgements
The authors acknowledge P.S. Wesson for his interesting comments. Furthermore, we acknowledge UNMdP and CONICET Argentina for financial support.
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Romero, J.M., Bellini, M. Induced Matter Theory of gravity from a Weitzenböck 5D vacuum and pre-big bang collapse of the universe. Eur. Phys. J. C 73, 2317 (2013). https://doi.org/10.1140/epjc/s10052-013-2317-x
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DOI: https://doi.org/10.1140/epjc/s10052-013-2317-x