Gravitational waves from electroweak phase transitions

By R. Apreda, M. Maggiore, Alberto Nicolis, A. Riotto. 2001

206 citations recorded by the source corpus.

Gravitational waves are generated during first-order phase transitions, either by turbulence or by bubble collisions. If the transition takes place at temperatures of the order of the electroweak scale, the frequency of these gravitational waves is today just within the band of the planned space interferometer LISA. We present a detailed analysis of the production of gravitational waves during an electroweak phase transition in different supersymmetric models where, contrary to the case of the Standard Model, the transition can be first order. We find that the stochastic background of gravitational waves generated by bubble nucleation can reach a maximum value View the MathML source of order (10−10–10−11), which is within the reach of the planned sensitivity of LISA, while turbulence can even produce signals at the level View the MathML source. These values of View the MathML source are obtained in the regions of the parameter space which can account for the generation of the baryon asymmetry at the electroweak scale.

View Paper: https://www.semanticscholar.org/paper/0611282735a6e80a1ca4226a02ef46ad4d7bd6ba

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Citations in the corpus

• Detecting gravitational waves from cosmological phase transitions with LISA: an update (2019, background): “Numerous analyses have investigated the EWPT in this setup before the LHC constraints on SUSY became as stringent [128–131].”
• On the maximal strength of a first-order electroweak phase transition and its gravitational wave signal (2018, background): “19)) and the parameter β/H [5–7], which yields the approximate timescale of the transition in terms of the Hubble parameter H.”
• Energy budget of cosmological first-order phase transitions (2010, unknown): “In [7] it was argued that the velocity should be fixed by the Chapman-Jouguet condition, like in chemical combustion, and this condition was subsequently used in many studies of gravitational wave production [8].”
• 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.”
• The Gravitational-Wave Physics (2017, methodology): “The capability of detecting GWs from PTs in Minimal Supersymmetric Standard Model (MSSM) and Next-to-Minimal Supersymmetric Standard Model (NMSSM) were first estimated in [111] and further explored in [112].”
• CosmoTransitions: Computing cosmological phase transition temperatures and bubble profiles with multiple fields (2011, methodology): “r at the origin. 2.1. One-dimensional solution When the eld has only one dimension, the solution to the critical bubble prole can easily be solved by the overshoot/undershoot method (see, e.g., Ref. [35]). Here, it is easiest to think of the problem as that of a classical particle moving under the i”
• Phase transitions in an expanding universe: stochastic gravitational waves in standard and non-standard histories (2020, background): “A further simplification says that Tn is determined by S3(Tn)/Tn = 140 [97].”
• Some cosmological implications of hidden sectors (2008, background): “When the bubbles finally percolate and collide, this energy is partially released into gravitational waves [22, 23, 24, 25].”