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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> 24<br />

When the Universe becomes dominated by dark energy (Λ > 0) the Hubble<br />

parameter becomes constant in time (cf. expression 19)<br />

<br />

Λ<br />

H(t) =c . (65)<br />

3<br />

Since inflation only lasts a few e–folds (see Section 1.3), the Hubble parameter<br />

can be taken as a constant during this period (e.g. Huang, 2007; Narlikar &<br />

Padmanabhan, 1991). From equation (40) we have<br />

H(t) = N(te)<br />

. (66)<br />

te<br />

Considering the normalisation (61) we can determine the proportionality constant<br />

in expression (19), yielding, for the scale factor of a Universe dominated<br />

by a positive cosmological constant, the result 9<br />

<br />

R(t) = exp c<br />

Λ<br />

3<br />

<br />

(t − t0) , tSN ≤ t ≤ t0 (67)<br />

where t0 is the present time (i.e. the age of the Universe) <strong>and</strong> tSN is the age<br />

of the universe at matter–Λ equality (corresponding to the instant when the<br />

expansion starts to accelerate). The dark energy domination is preceded by a<br />

matter–dominated stage which started when photons decoupled from matter.<br />

During matter domination the scale factor behaves according to expression (18).<br />

Considering that R(t) is a continuous function of time we will write, for the<br />

matter–dominated stage<br />

<br />

Λ<br />

R(t) = exp c 3 (tSN<br />

2/3 t − t0)<br />

, teq ≤ t ≤ tSN (68)<br />

tSN<br />

where teq is the age of the Universe at radiation–matter equality. Before that<br />

time, the Universe was radiation–dominated up to the end of inflation at some<br />

instant t = te. During radiation domination the scale factor behaves according<br />

to expression (17). During the period (te ≤ t ≤ teq) the Universe experienced<br />

two phase transitions during which it might have been, for brief instants, dust–<br />

like (Section 2). When one goes backwards in time the first phase transition<br />

is the QCD. Considering that t+ corresponds to the age of the Universe at the<br />

end of the QCD we write<br />

<br />

Λ<br />

R(t) = exp c 3 (tSN<br />

2/3 1/2 teq t<br />

− t0)<br />

, t+ ≤ t ≤ teq (69)<br />

tSN teq<br />

9 To our best knowledge, this sequence of formulae (equations 67–77) has never been deducted<br />

in the literature, although common-knowledge.

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