scholarly journals Gravitational wave energy budget in strongly supercooled phase transitions

2019 ◽  
Vol 2019 (06) ◽  
pp. 024-024 ◽  
Author(s):  
John Ellis ◽  
Marek Lewicki ◽  
José Miguel No ◽  
Ville Vaskonen
Keyword(s):  
Phase Transitions ◽  
Gravitational Wave ◽  
Energy Budget ◽  
Wave Energy

scholarly journals Energy budget and the gravitational wave spectra beyond the bag model

2021 ◽  
Vol 103 (10) ◽  
Author(s):  
Xiao Wang ◽  
Fa Peng Huang ◽  
Xinmin Zhang
Keyword(s):  
Gravitational Wave ◽  
Energy Budget ◽  
Wave Spectra ◽  
Bag Model

scholarly journals General properties of the gravitational wave spectrum from phase transitions

2009 ◽  
Vol 79 (8) ◽  
Author(s):  
Chiara Caprini ◽  
Ruth Durrer ◽  
Thomas Konstandin ◽  
Géraldine Servant
Keyword(s):  
Phase Transitions ◽  
Gravitational Wave ◽  
Wave Spectrum ◽  
General Properties

scholarly journals Gravitational wave energy spectrum of hyperbolic encounters

2012 ◽  
Vol 86 (4) ◽  
Author(s):  
Lorenzo De Vittori ◽  
Philippe Jetzer ◽  
Antoine Klein
Keyword(s):  
Energy Spectrum ◽  
Gravitational Wave ◽  
Wave Energy ◽  
Wave Energy Spectrum

scholarly journals Gravitational wave spectra from strongly supercooled phase transitions

2020 ◽  
Vol 80 (11) ◽  
Author(s):  
Marek Lewicki ◽  
Ville Vaskonen
Keyword(s):  
Phase Transitions ◽  
Scalar Field ◽  
Gravitational Wave ◽  
Low Frequency ◽  
Thin Wall ◽  
Omega 3 ◽  
Complex Scalar ◽  
High Frequencies ◽  
Field Gradients ◽  
Complex Scalar Field

AbstractWe study gravitational wave (GW) production in strongly supercooled cosmological phase transitions, taking particular care of models featuring a complex scalar field with a U(1) symmetric potential. We perform lattice simulations of two-bubble collisions to properly model the scalar field gradients, and compute the GW spectrum sourced by them using the thin-wall approximation in many-bubble simulations. We find that in the U(1) symmetric case the low-frequency spectrum is $$\propto \omega $$ ∝ ω whereas for a real scalar field it is $$\propto \omega ^3$$ ∝ ω 3 . In both cases the spectrum decays as $$\omega ^{-2}$$ ω - 2 at high frequencies.

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