Cosmological perturbations and the transition from contraction to expansion

Details Cosmological perturbations and the transition from contraction to expansion Cosmological perturbations and the transition from contraction to expansion

2003-01-24

arxiv.org/abs/hep-th/0301198v2

Phys.Rev. D67 (2003) 103517

Physics

High Energy Physics

High Energy Physics - Theory

30 pages, 16 figures. Version to appear in Phys. Rev. D. Slight modifications, but no change in the conclusion

Scientific paper

10.1103/PhysRevD.67.103517

We investigate both analytically and numerically the evolution of scalar perturbations generated in models which exhibit a smooth transition from a contracting to an expanding Friedmann universe. We find that the resulting spectral index in the late radiation dominated universe depends on which of the $\Psi$ or \$zeta$ variables passes regularly through the transition. The results can be parameterized through the exponent $q$ defining the rate of contraction of the universe. For $q \geq -1/2$ we find that there are no stable cases where both variables are regular during the transition. In particular, for $0

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