Gravitational Radiation From Cosmological Turbulence

By A. Kosowsky, A. Mack, T. Kahniashvili. 2001

250 citations recorded by the source corpus.

An injection of energy into the early Universe on a given characteristic length scale will result in turbulent motions of the primordial plasma. We calculate the stochastic background of gravitational radiation arising from a period of cosmological turbulence, using a simple model of isotropic Kolmogoroff turbulence produced in a cosmological phase transition. We also derive the gravitational radiation generated by magnetic fields arising from a dynamo operating during the period of turbulence. The resulting gravitational radiation background has a maximum amplitude comparable to the radiation background from the collision of bubbles in a first-order phase transition, but at a lower frequency, while the radiation from the induced magnetic fields is always subdominant to that from the turbulence itself. We briefly discuss the detectability of such a signal.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/92693628f568ff7fa6e51d6b8208774214677282

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. Marek Lewicki
2. C. Caprini
3. John Ellis
4. J. No
5. G. Servant
6. T. Konstandin
7. R. Durrer
8. M. Hindmarsh

In Nuclear and High Energy Physics

1. C. Caprini
2. T. Konstandin
3. G. Servant
4. R. Durrer
5. Marek Lewicki
6. John Ellis
7. J. No
8. M. Hindmarsh

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]).”
• Cosmological backgrounds of gravitational waves and eLISA/NGO: phase transitions, cosmic strings and other sources (2012, unknown): “The problem has been re-analysed later on in Kosowsky et al 2002 [27] and Dolgov et al 2002 [28], which both go beyond the quadrupole approximation directly integrating the GW equation (4), and both remark that since the turbulence arises in a fully ionised plasma, it has to be treated as MHD…”
• Gravitational waves from first order cosmological phase transitions in the Sound Shell Model (2019, background): “The leading term in the shear stress UETC is then [44–46]”
• 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]–[24] or preheating after inflation [25]–[30].”
• On the maximal strength of a first-order electroweak phase transition and its gravitational wave signal (2018, methodology): “In both scenarios we obtain the GW spectrum produced by sound waves [46–48] and plasma turbulence [49–53].”
• The stochastic gravitational wave background from turbulence and magnetic fields generated by a first-order phase transition (2009, methodology): “Previous analyses had either considered only the Kolmogorov range, ignoring the large scale part of the spectrum and continuing the Kolmogorov slope up to the peak [15, 16, 18, 20], or joined the two behaviors at the peak [17].”
• Science with the space-based interferometer eLISA. II: gravitational waves from cosmological phase transitions (2015, background): “[30], its contribution to the GW spectrum in eq.”
• Relic backgrounds of gravitational waves from cosmic turbulence (2002, methodology): “[4] underestimates the GW energy density by a factor of 4.”