Abstract
We study the gravitational wave phenomenology in models of solitosynthesis. In such models, a first order phase transition is precipitated by a period in which non-topological solitons with a conserved global charge (Q-balls) accumulate charge. As such, the nucleation rate of critical bubbles differs significantly from thermal phase transitions. In general we find that the peak amplitude of the gravitational wave spectrum resulting from solitosynthesis is stronger than that of a thermal phase transition and the timescale of the onset of nonlinear plasma dynamics is comparable to Hubble. We demonstrate this explicitly in an asymmetric dark matter model, and discuss current and future constraints in this scenario.
Highlights
Solitosynthesis [1] of Q-balls may result in a first order phase transition of a distinct kind [2,3,4]
We study the gravitational wave phenomenology in models of solitosynthesis
In general we find that the peak amplitude of the gravitational wave spectrum resulting from solitosynthesis is stronger than that of a thermal phase transition, while the timescale of the onset of nonlinear plasma dynamics may be comparable to Hubble
Summary
Solitosynthesis [1] of Q-balls may result in a first order phase transition of a distinct kind [2,3,4]. The scalar vacuum expectation value inside a Q-ball can reach the vicinity of the true vacuum In this case, Q-balls can grow through the accretion of global charge due to solitosynthesis (a process similar to nucleosynthesis) until a critical size is reached. Q-balls can grow through the accretion of global charge due to solitosynthesis (a process similar to nucleosynthesis) until a critical size is reached At this size the available free energy drives them to expand, completing the phase transition to the true vacuum. The resulting stochastic background spectrum depends solely on a few thermodynamic parameters: the temperature at which bubbles nucleate (or coalesce), the rate at which they nucleate, the velocity with which the bubble walls expand, and the amount of energy released to the surrounding plasma For this reason, the phenomenology of different microphysical models may be very similar. We derive how to calculate thermal parameters needed for gravitational wave phenomenology, before performing calculations in an explicit example of an asymmetric dark matter model
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