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dc.contributor.authorGarcía-Bellido, Juan-
dc.contributor.authorGarcía Figueroa, Daniel-
dc.date.accessioned2008-06-30T18:36:07Z-
dc.date.available2008-06-30T18:36:07Z-
dc.date.issued2008-01-27-
dc.identifier.citation17th Workshop on General Relativity and Gravitation in Japan (2008)en_US
dc.identifier.urihttp://hdl.handle.net/10261/5461-
dc.description20 pages, 8 figures.-- To appear in the Proceedings of the 17th Workshop on General Relativity and Gravitation (JGRG17), Nagoya (Japan), 3-7 December 2007.-- arXiv:0801.4109v1 [gr-qc]en_US
dc.description.abstractThe reheating of the universe after hybrid inflation proceeds through the nucleation and subsequent collision of large concentrations of energy density in the form of bubble-like structures moving at relativistic speeds. This generates a significant fraction of energy in the form of a stochastic background of gravitational waves, whose time evolution is determined by the successive stages of reheating: First, tachyonic preheating makes the amplitude of gravity waves grow exponentially fast. Second, bubble collisions add a new burst of gravitational radiation. Third, turbulent motions finally sets the end of gravitational waves production. From then on, these waves propagate unimpeded to us. We find that the fraction of energy density today in these primordial gravitational waves could be significant for GUT scale models of inflation, although well beyond the frequency range sensitivity of gravitational wave observatories like LIGO, LISA or BBO. However, low-scale models could still produce a detectable signal at frequencies accessible to BBO or DECIGO. For comparison, we have also computed the analogous background from some chaotic inflation models and obtained similar results to those of other groups. The discovery of such a background would open a new observational window into the very early universe, where the details of the process of reheating could be explored. Thus, it could also serve as a new experimental tool for testing the Inflationary Paradigm.en_US
dc.description.sponsorshipThis work is supported in part by CICYT projects FPA2003-03801 and FPA2006-05807, by EU network "UniverseNet" MRTN-CT-2006-035863 and by CAM project HEPHACOS S-0505/ESP-0346. D.G.F. and A.S. acknowledge support from a FPU-Fellowship from the Spanish M.E.C. We also acknowledge use of the MareNostrum Supercomputer under project AECT-2007-1-0005.en_US
dc.format.extent549515 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoengen_US
dc.relation.ispartofseriesIFT-UAM/CSIC-08-05en_US
dc.rightsopenAccessen_US
dc.subjectBig Bangen_US
dc.subjectGravitational Wave Backgrounden_US
dc.subjectGeneral Relativity and Quantum Cosmologyen_US
dc.subjectAstrophysicsen_US
dc.subjectHigh Energy Physics - Phenomenologyen_US
dc.titleA new gravitational wave background from the Big Bangen_US
dc.typeComunicación de congresoen_US
dc.description.peerreviewedPeer revieweden_US
Appears in Collections:(IFT) Comunicaciones congresos
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