Worth the Effort? An Examination on the Effect of Higher Diligence Calculations of the Sound Shell Model

Abstract

The gravitational wave spectrum arising from using the full velocity profile is well known to differ qualitatively from analytic fits to a broken power law. Former studies have shown that unlike the uncertainties arising from thermal field theory, more diligence in the hydrodynamics can sometimes have limited benefit. However, this was shown in the context of broken power law fits. We test the benefits of some recent calculations in modeling the spectrum, including new developments in adjustments of the low frequency tail to be consistent with causality, but we use the full velocity profile. We find the spectral shape information has a heightened sensitivity to the speed of sound which can be demonstrated analytically, however for our benchmark model this still results in a modest difference. The reason for a heightened sensitivity is because the velocity at the boundary is quite sensitive to the speed of sound, which in turn means a small change to the speed of sound can have a large change to the shape of the velocity profile. Furthermore, even modest changes in the product $ακ$ can make non-trivial changes to the shape around the peak. Finally, there are many points where adjusting the infrared behavior to be consistent with causality is affecting the spectrum near its peak. All this implies that the spectrum is sensitive to five thermal parameters rather than four which gives hope that an observation of a gravitational wave spectrum from a first order cosmological phase transition could eventually give even more information about the underlying microphysics responsible.

Figures (7)

• Figure 1: Interpretation of the metrics used to quantify the differences between gravitational wave spectra. The left panel shows the relationship between the ratio of the target spectrum’s peak amplitude to the high-diligence result and the $\frac{\Delta \Omega}{\Omega}$. The right panel compares the normalized gravitational wave spectra for the chosen parameter set, illustrating cases with different values of the KL divergence.
• Figure 2: (Top) Comparison of the uncertainties in the peak amplitude of the gravitational wave spectra obtained using different computational approaches at various wall velocities; (Bottom) Comparison of the KL divergence of the gravitational wave spectral shapes for different computational approaches at various wall velocities.
• Figure 3: Comparison of gravitational wave spectra at the benchmark points of the xSM from Table \ref{['tab: BP']}. We have considered four different scalar masses as denoted on top of each plot. We also assumed two different wall velocities $v_w = 0.92$ and $v_w = 0.56$ in the left and right panels of above figure, respectively.
• Figure 4: (Left) Comparison of the uncertainties in the peak amplitude of the gravitational wave spectra resulting from the $\mu \nu$ model and the bag model at various wall velocities; (Right) Comparison of the KL divergence between the gravitational wave spectral shapes predicted by the $\mu \nu$ model and the bag model at various wall velocities.
• Figure 5: The comparison plot of gravitational wave spectra resulting from the $\mu \nu$ model and the bag model at the benchmark points of the xSM.