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dc.contributor.authorFenu, Elisa-
dc.contributor.authorGarcía Figueroa, Daniel-
dc.contributor.authorDurrer, Ruth-
dc.contributor.authorGarcía-Bellido, Juan-
dc.date.accessioned2009-10-19T16:36:55Z-
dc.date.available2009-10-19T16:36:55Z-
dc.date.issued2009-10-07-
dc.identifier.citationJournal of Cosmology and Astroparticle Physics (JCAP) 10(2009)005en_US
dc.identifier.issn1475-7516-
dc.identifier.urihttp://hdl.handle.net/10261/17777-
dc.description21 pages, 2 figures.-- Full-text version available Open Access at the journal site.en_US
dc.description.abstractGravitational waves were copiously produced in the early Universe whenever the processes taking place were sufficiently violent. The spectra of several of these gravitational wave backgrounds on subhorizon scales have been extensively studied in the literature. In this paper we analyze the shape and amplitude of the gravitational wave spectrum on scales which are superhorizon at the time of production. Such gravitational waves are expected from the self ordering of randomly oriented scalar fields which can be present during a thermal phase transition or during preheating after hybrid inflation. We find that, if the gravitational wave source acts only during a small fraction of the Hubble time, the gravitational wave spectrum at frequencies lower than the expansion rate at the time of production behaves as Ω(GW)(f) α f^3 with an amplitude much too small to be observable by gravitational wave observatories like LIGO, LISA or BBO. On the other hand, if the source is active for a much longer time, until a given mode which is initially superhorizon (kη* << 1), enters the horizon, for kη >~ 1, we find that the gravitational wave energy density is frequency independent, i.e. scale invariant. Moreover, its amplitude for a GUT scale scenario turns out to be within the range and sensitivity of BBO and marginally detectable by LIGO and LISA. This new gravitational wave background can compete with the one generated during inflation, and distinguishing both may require extra information.en_US
dc.description.sponsorshipDGF also acknowledges support from a FPU-Fellowship from the Spanish M.E.C., with ref. AP-2005-1092. This work is supported by the Swiss National Science Foundation. We also acknowledge financial support from the Madrid Regional Government (CAM) under the program HEP-HACOS P-ESP-00346, and the Spanish Science Research Ministry (MEC) under contract FPA2006-05807. DGF and JGB participate in the Consolider-Ingenio 2010 PAU (CSD2007-00060), as well as in the European Union Marie Curie Network "UniverseNet" under contract MRTN-CT-2006-035863.en_US
dc.format.extent1413836 bytes-
dc.format.mimetypeapplication/pdf-
dc.language.isoengen_US
dc.publisherInstitute of Physics Publishingen_US
dc.relation.ispartofseriesIFT-UAM/CSIC-09-34-
dc.relation.ispartofseriesCERN-PH-TH/2009-145-
dc.rightsopenAccessen_US
dc.subjectCosmological phase transitionsen_US
dc.subjectInflationen_US
dc.subjectGravitational waves / sourcesen_US
dc.titleGravitational waves from self-ordering scalar fieldsen_US
dc.typeartículoen_US
dc.identifier.doi10.1088/1475-7516/2009/10/005-
dc.description.peerreviewedPeer revieweden_US
dc.relation.publisherversionhttp://dx.doi.org/10.1088/1475-7516/2009/10/005en_US
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