Abstract
We 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 whereas for a real scalar field it is propto omega ^3. In both cases the spectrum decays as omega ^{-2} at high frequencies.
Highlights
The direct detection of gravitational waves (GWs) from a binary black hole merger by LIGO [1] marked the dawn of a new era in astrophysics and cosmology
We 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 studied the GW spectrum produced in a strongly supercooled phase transition
Summary
The direct detection of gravitational waves (GWs) from a binary black hole merger by LIGO [1] marked the dawn of a new era in astrophysics and cosmology. In this paper we approximate the GW spectrum from strongly supercooled phase transitions by first studying the scaling of the gradient energy in two-bubble collisions by lattice simulations and calculating the GW spectrum by performing many-bubble simulations in thin-wall approximation In this way we can efficiently perform large simulations with realistic behaviour of the GW source. We find that in this case the gradient energy quickly reaches an R−2 scaling after the collision, whereas for a real scalar field we find that the decay is much faster In the former case we find that the GW spectrum is near the bulk flow result, and in the latter case we find a GW spectrum that grows as ω3 at low frequencies and decays as ω−2 at high frequencies.
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