Gravitational wave energy budget in strongly supercooled phase transitions
By John Ellis, Marek Lewicki, J. No, V. Vaskonen. Journal of Cosmology and Astroparticle Physics, 2019
286 citations recorded by the source corpus.
We derive efficiency factors for the production of gravitational waves through bubble collisions and plasma-related sources in strong phase transitions, and find the conditions under which the bubble collisions can contribute significantly to the signal. We use lattice simulations to clarify the dependence of the colliding bubbles on their initial state. We illustrate our findings in two examples, the Standard Model with an extra |H|6 interaction and a classically scale-invariant U(1)B−L extension of the Standard Model. The contribution to the GW spectrum from bubble collisions is found to be negligible in the |H|6 model, whereas it can play an important role in parts of the parameter space in the scale-invariant U(1)B−L model. In both cases the sound-wave period is much shorter than a Hubble time, suggesting a significant amplification of the turbulence-sourced signal. We find, however, that the peak of the plasma-sourced spectrum is still produced by sound waves with the slower-falling turbulence contribution becoming important off-peak.
Subfields: Astronomy and Astrophysics, Atomic and Molecular Physics, and Optics
View Paper: https://www.semanticscholar.org/paper/63b7bd73c92051a0618701af826fd003db334d61
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Citations in the corpus
- Updated predictions for gravitational waves produced in a strongly supercooled phase transition (2020, background): “tz factor at which the equilibrium would be reached, eq (middle) and the bubble wall Lorentz factor at the time of collisions, (right). The black curves are the same as in Fig.1. As discussed in Ref. [60], an important quantity for the GW calculation is the fraction of the total released energy that”
- Bubble wall velocity: heavy physics effects (2020, background): “It can be estimated from the ratio of initial and final radii of the bubble and is approximately equal to [24, 28] γmax ' 2R∗ 3R0 ( 1− PLO ∆V ) .”
- Gravitational waves from first order cosmological phase transitions in the Sound Shell Model (2019, background): “H−1 n [12, 19, 20], showing up as changes in the shape of the gravitational power spectrum.”
- Gravitational waves from first-order cosmological phase transitions: lifetime of the sound wave source (2020, methodology): “cates the regions with longlived sound-waves for dierent bubble wall velocities. 5 Gravitational wave signals 5.1 Energy budget We now review the energy budget of the phase transition [74] (see also [64]), in order to discuss the implications of the results from the previous Sections for the product”
- Towards an all-orders calculation of the electroweak bubble wall velocity (2020, background): “[51], which amounts to using 〈∆pz/(γT )〉 FC,FO in place of 〈∆pz/(γT )〉 and neglecting the logarithmic term.”
- Phase transitions in an expanding universe: stochastic gravitational waves in standard and non-standard histories (2020, background): “1 we compare our result with the suppression factor recently proposed in [23] (see also [54, 55]).”
- Theoretical uncertainties for cosmological first-order phase transitions (2020, background): “0.083 √ α+0.73 , (3.3) where Ssw(f) encodes the frequency dependence; at the peak, Ssw(f) = 1. We estimate the outstanding factor in Eq. (3.2) , the timescale on which acoustic waves are active, from [147, 148] H∗tsw = 2(8π)1/3 √ 1 +α p 3ακfβ/H∗ . (3.4) Since we are interested in the variation of th”
- AION: an atom interferometer observatory and network (2019, unknown): “Our calculation includes GWs sourced by both sound waves (dash-dotted line) and turbulence in the primordial plasma (dotted line) [84].”