Relic backgrounds of gravitational waves from cosmic turbulence

By A. Dolgov, D. Grasso, Alberto Nicolis. 2002

135 citations recorded by the source corpus.

Turbulence may have been produced in the early universe by several nonequilibrium processes. Periods of cosmic turbulence may have left a detectable relic under the form of stochastic backgrounds of gravitational waves. In this paper we derive general expressions for the power spectrum of the expected signal. Extending previous works on the subject, we take into account the effects of a continuous energy injection power and of magnetic fields. Both effects lead to relevant deviations from the Kolmogoroff turbulence spectrum. We apply our results to determine the spectrum of gravity waves which may have been produced by neutrino inhomogeneous diffusion and during a first order phase transition. We show that in both cases the expected signal may be in the sensitivity range of the interferometer LISA.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/56cc4be2a2df86865f163eb74a3218408e82be83

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. C. Caprini
2. T. Konstandin
3. G. Servant
4. R. Durrer
5. R. Cai
6. S. Huber
7. P. Bin'etruy
8. A. Boh'e

In Nuclear and High Energy Physics

1. C. Caprini
2. T. Konstandin
3. R. Durrer
4. G. Servant
5. S. Huber
6. R. Cai
7. P. Bin'etruy
8. J. Dufaux

Citations in the corpus

• The Gravitational-Wave Physics (2017, background): “The early analysis [74, 75] involving MHD exhibits three problems [37]: large-scale problem (addressed in [76, 77]), time-evolution problem (persisted in [77] and addressed in [76]) and dispersion-relation problem (corrected in [76, 77]).”
• The stochastic gravitational wave background from turbulence and magnetic fields generated by a first-order phase transition (2009, methodology): “In previous works, the turbulent velocity power spectrum Pv(k, t) was either assumed to be given only by the inertial range k−11/3 [15, 16, 18, 20], or naively determined by intersecting the k2 behaviour at very small scales with the inertial range k−11/3 behaviour [17].”
• Gravitational wave production by collisions: more bubbles (2008, background): “Notice also that a flatter spectrum simplifies the distinction from other sources of stochastic gravitational waves, such as turbulence [21, 22, 23, 24] or preheating after inflation [25, 26, 27, 28, 29, 30].”
• Cosmological backgrounds of gravitational waves and eLISA/NGO: phase transitions, cosmic strings and other sources (2012, methodology): “Dolgov et al. 2002 [28] uses the result of [27] for the GW spectrum, but parametrically introduces also power-law deviations from the Kolmogorov spectrum, and generalises the analysis to the case when the time during which turbulence is active is of the order of the Hubble time.”