The end of thermal inflation proceeds by nucleating true-vacuum bubbles rather than by global phase mixing, and the resulting gravitational-wave background can reach BBO and DECIGO sensitivities for low flaton mass scale gamma.
Revisiting the envelope approximation: gravitational waves from bubble collisions
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abstract
We study the envelope approximation and its applicability to first-order phase transitions in the early universe. We demonstrate that the power laws seen in previous studies exist independently of the nucleation rate. We also compare the envelope approximation prediction to results from large-scale phase transition simulations. For phase transitions where the contribution to gravitational waves from scalar fields dominates over that from the coupled plasma of light particles, the envelope approximation is in agreement, giving a power spectrum of the same form and order of magnitude. In all other cases the form and amplitude of the gravitational wave power spectrum is markedly different and new techniques are required.
fields
hep-ph 2years
2026 2representative citing papers
Early matter domination with time-dependent decay rates produces multiple first-order phase transitions whose gravitational wave signatures encode the transition and reheating temperatures.
citing papers explorer
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Phase Transitions and Gravitational Wave Production at the End of Thermal Inflation
The end of thermal inflation proceeds by nucleating true-vacuum bubbles rather than by global phase mixing, and the resulting gravitational-wave background can reach BBO and DECIGO sensitivities for low flaton mass scale gamma.
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Gravitational Waves from Multiple First-Order Phase Transitions in a Scenario with Early Matter Domination
Early matter domination with time-dependent decay rates produces multiple first-order phase transitions whose gravitational wave signatures encode the transition and reheating temperatures.