Primordial Black Holes and Cosmological Phase Transitions Report ...

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PBHs and Cosmological Phase Transitions 216 12.2 Future work So far, we have determined the fraction of the universe going into PBHs, β(tk), during radiation domination and during cosmological phase transitions. Here we present some objectives and ideas for future work; in approximately chronological order: • We plan to determine the PBH distribution in the Universe based on the results obtained so far. There are two main possibilities: (a) the distribution of PBHs is homegeneous throught the entire universe and (b) PBHs are clustered around galactic halos. We want to explore both. • The existence of critical phenomena suggests that PBHs may be much smaller tant the particle horizon at formation with masses that might be as small as 10 −4 MH. We want to explore this subject and how it affects the PBH mass spectrum. • At this stage, the results should show some dependence on the model one uses for the spectrum of primordial density fluctuations. So far, we have concentrated mainly on a running–tilt power–law spectrum because it is highly supported by recent WMAP observations. However, even in this case, there is a strong lack of observational data. It is expected that upcoming missions, such as the Planck Satellite (planned to launch in April 2009), could provide some of these data. • We plan to work aslo with other types of spectra (e.g. broken scale invariance spectrum) and compare the results with the ones achieved so far. • When a PBH forms at a given epoch it could swallow smaller mass PBHs existing in the neighboord. We plan to study the importance of this process and evaluate how it affects the values of β(k). • If PBHs are created highly clustered, then this could lead to a huge number of PBH binaries and also to a huge number of PBH mergers (which would lead to the formation of bigger BHs). We plan to determine how this could affect the density distribution function of PBHs on the universe, possibly through simulations. • In the not so near future we want to improve our results considering a single model accounting for all these ideas. We also want to extend our study to the period between the end of inflation ∼ 10 −33 s and 10 −23 s.
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Contents List of Figures vii List o
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List of Tables 1 The Universe timel
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