Loop Quantum Gravity Effective Matter Dynamics

Details Loop Quantum Gravity Effective Matter Dynamics Loop Quantum Gravity Effective Matter Dynamics

Dec 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002nmgm.meet.1265a&link_type=abstract

"THE NINTH MARCEL GROSSMANN MEETING On Recent Developments in Theoretical and Experimental General Relativity, Gravitation and R

Physics

Scientific paper

The cosmological character of Gamma-Ray-Bursts 1 (GRBs), short and intense bursts of 100 keV - 1 MeV photons and 105 - 109 GeV neutrinos 2, makes it plausible to probe quantum gravity -which is expected to become important near Planck scale: EQG ˜ EP : = √ {\hbar c5 /G} ≈ 1019 {GeV}. To see why one can look at -for instance- dispersion relations for photons in a space endowed with a structure required by an underlying quantum gravity theory3, say c2 {bar p2} /E2 = 1 + ξ E/EQG + {O} (E/EQG )2 with ξ a parameter of order one, E the energy and vec p the spatial momentum of the photon. The result is a speed v/c = (1/c)∂ E/∂ p = 1 - ξ E/EQG + {O} (E/EQG )2 , and a retardation time w.r.t. to speed c propagation: Δt ≈ ξ(E/EQG)(L/c), L being the distance traveled. With E ≈ 0.20MeV, L ≈ 1010ly, one gets Δt ≈ 10-5s. This can be contrasted with the time resolution of GRBs δt ≈ 10-3s. Indeed, effective dispersion relations might have observable imprints of physics at Planck scale and may be other aspects of quantum gravity can be probed7. Here we point out how non perturbative quantum general relativity can yield such effective dispersion relations either for photons or neutrinosa...

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