Big bounce from spin and torsion

Nikodem J. Poplawski

doi:10.1007/s10714-011-1323-2

paper

Big bounce from spin and torsion

arXiv:1105.6127 · doi:10.1007/s10714-011-1323-2

Abstract

The Einstein-Cartan-Sciama-Kibble theory of gravity naturally extends general relativity to account for the intrinsic spin of matter. Spacetime torsion, generated by spin of Dirac fields, induces gravitational repulsion in fermionic matter at extremely high densities and prevents the formation of singularities. Accordingly, the big bang is replaced by a bounce that occurred when the energy density $ε \propto g T^{4}$ was on the order of $n^{2} / m_{Pl}^{2}$ (in natural units), where $n \propto g T^{3}$ is the fermion number density and $g$ is the number of thermal degrees of freedom. If the early Universe contained only the known standard-model particles ( $g \approx 100$ ), then the energy density at the big bounce was about 15 times larger than the Planck energy. The minimum scale factor of the Universe (at the bounce) was about $1 0^{32}$ times smaller than its present value, giving $\approx 50 \mum$. If more fermions existed in the early Universe, then the spin-torsion coupling causes a bounce at a lower energy and larger scale factor. Recent observations of high-energy photons from gamma-ray bursts indicate that spacetime may behave classically even at scales below the Planck length, supporting the classical spin-torsion mechanism of the big bounce. Such a classical bounce prevents the matter in the contracting Universe from reaching the conditions at which a quantum bounce could possibly occur.

6 pages; published version

Big bounce from spin and torsion

Abstract

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