Amplification of Vacuum Fluctuations in String Cosmology Backgrounds

Inflationary string cosmology backgrounds can amplify perturbations in a more efficient way than conventional inflationary backgrounds, because the perturbation amplitude may grow instead of being constant outside the horizon. If not gauged away, the growing mode can limit the range of validity of a linearized description of perturbations. Even in the restricted linear range, however, this enhanced amplification may lead to phenomenological consequences unexpected in the context of the standard inflationary scenario. In particular, the production of a relic graviton background strong enough to be detected in future by LIGO, and/or the generation of a stochastic electromagnetic background strong enough to seed the cosmic magnetic fields and to be responsible for the observed large scale anisotropy. * Talk given at the “3rd Colloque Cosmologie” (Observatoire de Paris, 7-9 June 1995). To appear in the Proceedings (World Scientific, Singapore), ed. by H. de Vega and N. Sanchez. AMPLIFICATION OF VACUUM FLUCTUATIONS IN STRING COSMOLOGY BACKGROUNDS M. GASPERINI Dipartimento di Fisica Teorica, Università di Torino, Via P.Giuria 1, 10125 Turin, Italy, and INFN, Sezione di Torino, Turin, Italy ABSTRACT Inflationary string cosmology backgrounds can amplify perturbations in a more efficient way than conventional inflationary backgrounds, because the perturbation amplitude may grow instead of being constant outside the horizon. If not gauged away, the growing mode can limit the range of validity of a linearized description of perturbations. Even in the restricted linear range, however, this enhanced amplification may lead to phenomenological consequences unexpected in the context of the standard inflationary scenario. In particular, the production of a relic graviton background strong enough to be detected in future by LIGO, and/or the generation of a stochastic electromagnetic background strong enough to seed the cosmic magnetic fields and to be responsible for the observed large scale anisotropy.