Primordial Black Holes and Cosmological Phase Transitions Report ...
Primordial Black Holes and Cosmological Phase Transitions Report ... Primordial Black Holes and Cosmological Phase Transitions Report ...
PBHs and Cosmological Phase Transitions 164 Table 36: The evolution of δc1 as a function of time for a EW Crossover with ∆T =0.013Tc when δc =1/3. log 10(tk/1 s) δc1 log 10(tk/1 s) δc1 -10.2 0.33333 -10.1 0.33205 -10.0 0.33221 -9.9 0.33254 -9.8 0.33277 -9.7 0.33293 -9.6 0.33305 -9.5 0.33313 -9.4 0.33319 -9.3 0.33323 -9.2 0.33326 -9.1 0.33328 -9.0 0.33330 -8.9 0.33331 -8.8 0.33332 -8.7 0.33332 -8.6 0.33332 -8.5 0.33333 fraction of the overdense region spent in the dust–like phase, will be given, once again, by expressions (254) to (258), in accordance with the class of fluctuation we are dealing with. For the QCD Bag Model case we have studied with some detail fluctuations crossing the horizon before the mixed phase (Section 7.1.1), during the mixed phase (Section 7.1.2) and after the mixed phase (Section 7.1.3). Here, in the EW Bag Model case, we just point out that one obtains similar results. For example, one should obtain situations similar to the ones represented on Figure 51 (naturally with different values for x, δc1, δc2,...). On Figure 86a we show the region in the (x, δ) plane for which BH formation is allowed in the case δc =1/3. Without the phase transition this would be a straight horizontal line at δ =1/3. On Figure 86b we show the same situation but now represented on the (log 10(t),δ). We have represented also, for reference, the values tEW− and tEW+. On Figure 87 we show the region in the (log 10 (t),δ) plane for which BH formation is allowed in the case δc =0.7. Without the phase transition this would be a straight horizontal line at δ =0.7. On Table 37 we present the new values for the threshold of PBH formation during a EW first–order phase transition within the MSSM according to the Bag Model for the case δc =1/3.
PBHs and Cosmological Phase Transitions 165 ∆ ∆ 1.2 1 0.8 0.6 0.4 0.2 1.2 0.8 0.6 0.4 ∆c1 ∆c2 a No BH formation BH formation ∆c13 No BH formation 0 20 40 60 80 100 x b 1 No BH formation ∆c13 BH formation ∆c2 tEW tEW 0.2 ∆c1 No BH formation -11 -10.5 -10 -9.5 Log10t1s Figure 86: The curve indicating which parameter values lead to collapse to a BH when δc =1/3 during the EW transition within the MSSM: (a) in the (x, δ) plane; (b) in the (log 10(t/1 s),δ) plane.
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- Page 221 and 222: Table 49 (continued). PBHs and Cosm
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PBHs <strong>and</strong> <strong>Cosmological</strong> <strong>Phase</strong> <strong>Transitions</strong> 165<br />
∆<br />
∆<br />
1.2<br />
1<br />
0.8<br />
0.6<br />
0.4<br />
0.2<br />
1.2<br />
0.8<br />
0.6<br />
0.4<br />
∆c1<br />
∆c2<br />
a<br />
No BH formation<br />
BH formation<br />
∆c13<br />
No BH formation<br />
0 20 40 60 80 100<br />
x<br />
b<br />
1<br />
No BH formation<br />
∆c13<br />
BH formation<br />
∆c2<br />
tEW<br />
tEW<br />
0.2<br />
∆c1<br />
No BH formation<br />
-11 -10.5 -10 -9.5<br />
Log10t1s Figure 86: The curve indicating which parameter values lead to collapse to a<br />
BH when δc =1/3 during the EW transition within the MSSM: (a) in the (x, δ)<br />
plane; (b) in the (log 10(t/1 s),δ) plane.
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