Gravitational wave production by collisions: more bubbles

By S. Huber, T. Konstandin. 2008

509 citations recorded by the source corpus.

We re-examine the production of gravitational waves by bubble collisions during a first-order phase transition. The spectrum of the gravitational radiation is determined by numerical simulations using the ‘envelope approximation’. We find that the spectrum rises as f3.0 for small frequencies and decreases as f−1.0 for high frequencies. Thus, the fall-off at high frequencies is significantly slower than previously stated in the literature. This result has direct impact on detection prospects for gravity waves originating from a strong first-order electroweak phase transition at space-based interferometers, such as LISA and BBO. In addition, we observe a slight dependence of the peak frequency on the bubble wall velocity.

View Paper: https://www.semanticscholar.org/paper/e8490b79fbf615e60ada14fd4c6bd039fb00f2cd

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Citations in the corpus

• Gravitational wave energy budget in strongly supercooled phase transitions (2019, background): “However, more recently such scenarios have enjoyed renewed attention due to the observational prospects associated with a gravitational wave (GW) background that such a transition could produce [5–44] 1.”
• Cosmological backgrounds of gravitational waves and eLISA/NGO: phase transitions, cosmic strings and other sources (2012, methodology): “Shortly after the analytical estimation of [24], Huber and Konstandin 2008 [26] simulated again the collision of bubbles in the envelope approximation, with considerably improved numerical accuracy, which allows to determine a larger portion of the spectrum and consequently a more careful analysis…”
• Gravitational waves from first order cosmological phase transitions in the Sound Shell Model (2019, background): “The sound shell model does not apply in the run-away scenario; the so-called envelope approximation [36, 37] gives an order-of-magnitude estimate of the gravitational wave power.”
• Cosmological Magnetic Fields: Their Generation, Evolution and Observation (2013, methodology): “This result has been obtained with numerical simulations, see Kamionkowski et al (1994); Huber and Konstandin (2008).”
• Updated predictions for gravitational waves produced in a strongly supercooled phase transition (2020, background): “Initially these walls were assumed simply to disappear upon collision as the energy dissipates [92–94].”
• Model-independent energy budget of cosmological first-order phase transitions—A sound argument to go beyond the bag model (2020, background): “energy density in the fluid [37] (if turbulence develops in less than a Hubble time, this relation can be modified [23]).”
• Gravitational waves from bubble dynamics: beyond the envelope (2017, methodology): “ approximation," in which the released energy is assumed to be concentrated in innitely thin bubble walls.}1 Later a numerical simulation with the same approximations has been performed in Ref. [70] with an increased number of bubbles, and a more precise form of the GW spectrum has been obtaine”
• Dark, cold, and noisy: constraining secluded hidden sectors with gravitational waves (2018, background): “Reference [54] [55] [57]”
• Some cosmological implications of hidden sectors (2008, background): “Considering that the GW spectrum from collisions scales approximately as h(2)Ω ∝ 1/f for large frequencies [25], one obtains for BBO a signal to sensitivity ratio 1.”
• Science with the space-based interferometer eLISA. II: gravitational waves from cosmological phase transitions (2015, methodology): “3 Numerical simulations utilizing the envelope approximation suggest that the GW contribution to the spectrum is given by [16]”
• The stochastic gravitational wave background from turbulence and magnetic fields generated by a first-order phase transition (2009, methodology): “19) has been introduced to mimic the turning on of the source in the bubble collision case, inferred from numerical simulations, see [13].”