Energy budget of cosmological first-order phase transitions

By J. Espinosa, T. Konstandin, J. No, G. Servant. 2010

608 citations recorded by the source corpus.

The study of the hydrodynamics of bubble growth in first-order phase transitions is very relevant for electroweak baryogenesis, as the baryon asymmetry depends sensitively on the bubble wall velocity, and also for predicting the size of the gravity wave signal resulting from bubble collisions, which depends on both the bubble wall velocity and the plasma fluid velocity. We perform such study in different bubble expansion regimes, namely deflagrations, detonations, hybrids (steady states) and runaway solutions (accelerating wall), without relying on a specific particle physics model. We compute the efficiency of the transfer of vacuum energy to the bubble wall and the plasma in all regimes. We clarify the condition determining the runaway regime and stress that in most models of strong first-order phase transitions this will modify expectations for the gravity wave signal. Indeed, in this case, most of the kinetic energy is concentrated in the wall and almost no turbulent fluid motions are expected since the surrounding fluid is kept mostly at rest.

Subfields: Astronomy and Astrophysics, Nuclear and High Energy Physics

View Paper: https://www.semanticscholar.org/paper/8dff5075e4b2dec42e3d5f9af056323b6705ba70

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. John Ellis
3. C. Caprini
4. J. No
5. T. Konstandin
6. V. Vaskonen
7. G. Servant
8. M. Hindmarsh

In Nuclear and High Energy Physics

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

Citations in the corpus

• Reconstructing the spectral shape of a stochastic gravitational wave background with LISA (2019, background): “a kination dominated phase [46–50], non-perturbative particle production phenomena [51–62], oscillon dynamics [63–67], strong first order phase transitions [68–81], or cosmic defect networks [82–93].”
• Cosmological Magnetic Fields: Their Generation, Evolution and Observation (2013, background): “This is a typical number found in numerical simulations by Huber and Konstandin (2008), but it depends sensitively on the strength of the phase transition (Caprini et al 2008; Espinosa et al 2010).”
• Gravitational wave energy budget in strongly supercooled phase transitions (2019, methodology): “We also define [56] (see also [57])”
• Model-independent energy budget of cosmological first-order phase transitions—A sound argument to go beyond the bag model (2020, methodology): “of the phase transition properly and the fits to the efficiency coefficient in the bag model [29] apply.”
• Challenges and opportunities of gravitational-wave searches at MHz to GHz frequencies (2020, background): “They can also be fundamental strings (14)Approximate fits can be found in [194].”
• Gravitational waves from first order cosmological phase transitions in the Sound Shell Model (2019, background): “[31], and is included for ease of reference.”
• Dark, cold, and noisy: constraining secluded hidden sectors with gravitational waves (2018, background): “For a phase transition in a hidden sector, α∞ is given by [5, 40]”
• Science with the space-based interferometer eLISA. II: gravitational waves from cosmological phase transitions (2015, methodology): “The following picture emerges in this case [9].”
• Cosmological backgrounds of gravitational waves and eLISA/NGO: phase transitions, cosmic strings and other sources (2012, methodology): “For the first time the bubble wall velocity vb and the efficiency factor κ have been evaluated beyond the Jouguet detonation hypothesis, adopting the complete model for bubble propagation developed in Espinosa et al. 2010 [23].”