Gravitational waves and the scale of inflation
- Institute for Advanced Study, Princeton, NJ (United States)
- Stanford Univ., Stanford, CA (United States)
Here, we revisit alternative mechanisms of gravitational wave production during inflation and argue that they generically emit a non-negligible amount of scalar fluctuations. We find the scalar power is larger than the tensor power by a factor of order 1/ε2. For an appreciable tensor contribution, the associated scalar emission completely dominates the zero-point fluctuations of the inflaton, resulting in a tensor-to-scalar ratio r ~ ε2. A more quantitative result can be obtained if one further assumes that gravitational waves are emitted by localized subhorizon processes, giving rmax ≃ 0.3ε2. However, ε is generally time dependent, and this result for r depends on its instantaneous value during the production of the sources, rather than just its average value, somewhat relaxing constraints from the tilt ns. We calculate the scalar 3-point correlation function in the same class of models and show that non-Gaussianity cannot be made arbitrarily small, i.e. fNL ≳ 1, independently of the value of r. Possible exceptions in multifield scenarios are discussed.
- Research Organization:
- Stanford Univ., CA (United States)
- Sponsoring Organization:
- USDOE Office of Science (SC), High Energy Physics (HEP)
- Grant/Contract Number:
- SC0008078; FG02-12ER41854
- OSTI ID:
- 1491084
- Alternate ID(s):
- OSTI ID: 1180012
- Journal Information:
- Physical Review. D, Particles, Fields, Gravitation and Cosmology, Vol. 91, Issue 6; ISSN 1550-7998
- Publisher:
- American Physical Society (APS)Copyright Statement
- Country of Publication:
- United States
- Language:
- English
Web of Science
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