Stochastic gravitational background from inflationary phase transitions
We consider true vacuum bubbles generated in a first order phase transition occurring during the slow rolling era of a two field inflation: it is known that gravitational waves are produced by the collision of such bubbles. We find that the epoch of the phase transition strongly affects the characte...
Gespeichert in:
| Hauptverfasser: | , |
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| Dokumenttyp: | Article (Journal) |
| Sprache: | Englisch |
| Veröffentlicht: |
15 October 1997
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| In: |
Physical review. D, Particles, fields, gravitation, and cosmology
Year: 1997, Jahrgang: 56, Heft: 8, Pages: 4610-4617 |
| ISSN: | 1550-2368 |
| DOI: | 10.1103/PhysRevD.56.4610 |
| Online-Zugang: | Verlag, Volltext: http://dx.doi.org/10.1103/PhysRevD.56.4610 Verlag, Volltext: https://link.aps.org/doi/10.1103/PhysRevD.56.4610 
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| Verfasserangaben: | Carlo Baccigalupi, Luca Amendola, Pierluigi Fortini and Franco Occhionero |
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| 245 | 1 | 0 | |a Stochastic gravitational background from inflationary phase transitions |c Carlo Baccigalupi, Luca Amendola, Pierluigi Fortini and Franco Occhionero |
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| 520 | |a We consider true vacuum bubbles generated in a first order phase transition occurring during the slow rolling era of a two field inflation: it is known that gravitational waves are produced by the collision of such bubbles. We find that the epoch of the phase transition strongly affects the characteristic peak frequency of the gravitational waves, causing an observationally interesting redshift in addition to the post-inflationary expansion. In particular it is found that a phase transition occurring typically 10-20 e-foldings before the reheating at kT≃1015GeV may be detected by the next LIGO gravity waves interferometers. Moreover, for recently proposed models capable of generating the observed large scale voids as remnants of the primordial bubbles (for which the characteristic wave lengths are several tens of Mpc), it is found that the level of anisotropy of the cosmic microwave background provides a deep insight upon the physical parameters of the effective Lagrangian. | ||
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