190 likes | 396 Views
A strained space-time. Angelo Tartaglia DIFIS, Politecnico di Torino and INFN. r. r’. X a. “Elastic” continua. N+n. N. ξ a. x μ. N. Space-time defect. Flat reference frame. Curved natural frame. Strained space-time. unstrained. dr 0. . Strain tensor. g . dr. strained.
E N D
A strained space-time Angelo Tartaglia DIFIS, Politecnico di Torino and INFN
r r’ Xa “Elastic” continua N+n N ξa xμ N ERE2010 - Granada
Space-time defect Flat reference frame Curved natural frame ERE2010 - Granada
Strained space-time unstrained dr0 Strain tensor g dr strained ERE2010 - Granada
The Lagrangian density Potential term “Kinetic”term Geometry ERE2010 - Granada
l r z l r Robertson-Walker symmetry =f(r) ERE2010 - Granada
The Hubble parameter A. Tartaglia and N. Radicella, CQG, 27, 035001 (2010) ERE2010 - Granada
Fitting the data (307 SnIa) ERE2010 - Granada 8
Other cosmological tests • Primordial nucleosynthesis (correct proportion between He, D and hydrogen) • CMB spectrum • Structure formation after the recombination era. ERE2010 - Granada
Bayesian posterior probability ERE2010 - Granada
Optimal value of the parameters N. Radicella, M. Sereno, A. Tartaglia ERE2010 - Granada
Schwarzschild symmetry Natural frame Reference frame (Minkowski) Gauge function ERE2010 - Granada
The strain tensor ERE2010 - Granada
Three field equations ERE2010 - Granada
Weak strain ERE2010 - Granada
Approximate solutions , = functions of , ~ , ERE2010 - Granada
Post-Keplerian circular orbits Looks like the effect of dark matter Light rays ERE2010 - Granada
Conclusion • The strained space-time theory introduces a strain energy of vacuum depending on curvature • The theory accounts for the accelerated expansion of the universe and is consistent with BBN, structure formation and SnIa’s • The strain affects free fall also in spherically symmetric stationary space-times ERE2010 - Granada