REVIEW 12 cited by
Gravitational waves from first order cosmological phase transitions in the Sound Shell Model
Not yet reviewed by Pith; the record is open.
This paper has not been read by Pith yet. Machine review is queued; the pith claim, tier, and objections will appear here once it completes.
SPECIMEN: schema-true, not a live event
T0 review · schema-true
One-sentence machine reading of the paper's core claim.
pith:XXXXXXXX · record.json · timestamp
read the original abstract
We calculate gravitational wave power spectra from first order early Universe phase transitions using the Sound Shell Model. The model predicts that the power spectrum depends on the mean bubble separation, the phase transition strength, the phase boundary speed, with the overall frequency scale set by the nucleation temperature. There is also a dependence on the time evolution of the bubble nucleation rate. The gravitational wave peak power and frequency are in good agreement with published numerical simulations, where bubbles are nucleated simultaneously. Agreement is particularly good for detonations, but the total power for deflagrations is predicted higher than numerical simulations show, indicating refinement of the model of the transfer of energy to the fluid is needed for accurate computations. We show how the time-dependence of the bubble nucleation rate affects the shape of the power spectrum: an exponentially rising nucleation rate produces higher amplitude gravitational waves at a longer wavelength than simultaneous nucleation. We present an improved fit for the predicted gravitational wave power spectrum in the form of a double broken power law, where the two breaks in the slope happen at wavenumber corresponding to the mean bubble separation and the thickness of the fluid shell surrounding the expanding bubbles, which in turn is related to the difference of the phase boundary speed from the speed of sound.
Forward citations
Cited by 12 Pith papers
-
Non-conformal obstructions to bubble expansion
Non-conformal equations of state introduce wall and flow obstructions that delete entire classes of bubble solutions and create 'shocked detonations', shrinking the allowed wall-velocity space and suppressing gravitat...
-
Can the universe be matter-dominated after a supercooled first-order phase transition?
After a supercooled first-order phase transition, the scalar field's equation of state is set by the bubble-wall Lorentz factor γ*, and matter domination is delayed until a/a* ≃ γ* in the free-streaming limit.
-
Gravitational Waves from Particles Produced from Bubble Collisions in First-Order Phase Transitions
Particles produced from bubble collisions generate a gravitational-wave signal whose low-frequency slope can dominate the standard signal from first-order phase transitions.
-
Consistent Thermal Resummation and Phase Transitions with 2PI Methods
A 2PI-Hartree effective potential for two mixing scalars is renormalized and used to show that self-consistent thermal resummation can substantially alter predicted phase transition strengths and gravitational wave spectra.
-
Strong First-Order Electroweak Phase Transitions and Gravitational Waves in the Normal Two-Higgs-Doublet Model: A Comparative Study of the Four Yukawa Types and Thermal Resummation Schemes
In the Normal 2HDM, SFOEWPTs are single-step and alignment-favoring across all four Yukawa types, yet Parwani versus Arnold–Espinosa resummation changes the viable heavy-mass range from ~1.6 TeV to ≲800 GeV and leaves...
-
Vacuum bubbles from cosmic ripples
Over-densities in the early universe reduce the Euclidean action for vacuum decay, making false-vacuum bubbles nucleate earlier; under-densities do the opposite.
-
Supercooled Phase Transitions: Why Thermal History of Hidden Sector Matters in Analysis of Pulsar Timing Array Signals
Tracking the evolving temperature ratio between hidden and visible sectors can change a supercooled hidden-sector phase transition's gravitational wave spectrum by up to four orders of magnitude, reviving it as an exp...
-
Thermalization effects on the dynamics of growing vacuum bubbles
Bubble-wall terminal velocity depends on plasma thermalization; non-equilibrium and free-streaming regimes give slower or different walls, and stationary solutions can be bypassed by runaways.
-
The price for monopole dark matter
Dark matter can consist of 't Hooft-Polyakov monopoles in a dark SU(2) sector, but only in a narrow window with m_M ≳ 10^8 GeV, near-bound dark radiation, and possibly detectable gravitational waves.
-
The art of simulating the early Universe. Part III: Scalar-Gauge-Fluid Dynamics
Detailed continuum-to-lattice schemes are given for perfect/imperfect fluids alone or coupled to scalars/gauges in FLRW, enabling self-consistent CosmoLattice simulations of early-Universe plasma dynamics and GWs.
-
Primordial Gravitational Waves from Phase Transitions during Reheating
Phase transitions happening during reheating can produce gravitational-wave signals that are delayed, prolonged, and shifted in amplitude and frequency by orders of magnitude compared with standard cosmology.
-
Gamma-Rays and Gravitational Waves from Inelastic Higgs Portal Dark Matter
An inelastic complex-scalar Higgs portal dark matter model can evade direct detection, explain the Galactic Center gamma-ray excess, and produce a first-order electroweak phase transition with a gravitational wave sig...
Discussion (0). Continue with ORCID to comment.