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Primordial Black Holes and Cosmological Phase Transitions Report ...

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PBHs <strong>and</strong> <strong>Cosmological</strong> <strong>Phase</strong> <strong>Transitions</strong> 65<br />

Figure 18: The Hubble rate H <strong>and</strong> the typical interaction rates of weak (Γw) <strong>and</strong><br />

electric (Γe) processes that involve relativistic particles, as well as the typical<br />

rate of a weak annihilation rate Γw,ann for a particle mass of 100 GeV. The<br />

dashed line indicates the rate 1/s. At tH ∼ 1s, the weak interaction rate falls<br />

below the expansion rate (chemical <strong>and</strong> kinetic decoupling of neutrinos, kinetic<br />

decoupling of neutralinos); at temperatures of the order of 1-10 GeV neutralinos<br />

freeze–out. The electric interaction rate stays well above the Hubble rate up<br />

to the epoch of photon decoupling, which occurs well after the epochs we show<br />

here (Schwarz, 2003).<br />

librium (LTE) depends on the comparison of two time scales: the cooling rate<br />

due to cosmological expansion (e.g. Boyanovsky et al., 2006)<br />

1 dT (t) 1 dR(t)<br />

= − = −H(t) (122)<br />

T (t) dt R(t) dt<br />

<strong>and</strong> the rate of equilibration Γ. LTE follows when Γ >H(t), in which case the<br />

evolution is adiabatic in the sense that the thermodynamic functions depend<br />

slowly on time through the temperature (e.g. Boyanovsky et al., 2006, see Figure<br />

18). Strong, electric, <strong>and</strong> weak interactions keep all relativistic particles in<br />

kinetic <strong>and</strong> chemical equilibrium down to temperatures of ∼ 1 MeV. At that<br />

point neutrinos <strong>and</strong> neutrons decouple chemically <strong>and</strong> kinetically from the rest<br />

of the radiation fluid (e.g. Schwarz, 2003).<br />

When the cosmological expansion is too fast (namely H(t) ≫ Γ) LTE cannot<br />

happen, the temperature drops too fast for the system to have time to relax to<br />

LTE <strong>and</strong> the phase transition occurs via a quench from the high into the low<br />

temperature phase (e.g. Boyanovsky et al., 2006).<br />

In the case of the QCD transition the isentropic condition applies after initial<br />

supercooling, bubble nucleation, <strong>and</strong> sudden reheating to Tc. During this part<br />

of the transition, which takes about 99% of the transition time, the fluid is<br />

extremely close to thermal equilibrium, because the time to reach equilibrium<br />

is very much shorter than a Hubble time, i.e. the fluid makes a reversible

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