Abstract
We in this paper investigate the formation and evolution of primordial black holes (PBHs) in nonsingular bouncing cosmologies. We discuss the formation of PBH in the contracting phase and calculate the PBH abundance as a function of the sound speed and Hubble parameter. Afterwards, by taking into account the subsequent PBH evolution during the bouncing phase, we derive the density of PBHs and their Hawking radiation. Our analysis shows that nonsingular bounce models can be constrained from the backreaction of PBHs.
Highlights
The matter bounce scenario [1,2,3] is one type of nonsingular bounce cosmology [4,5,6,7,8,9], which is often viewed as an important alternative to the standard inflationary paradigm [10,11,12,13]
We in this paper investigate the formation and evolution of primordial black holes (PBHs) in nonsingular bouncing cosmologies
Our analysis shows that nonsingular bounce models can be constrained from the backreaction of PBHs
Summary
The matter bounce scenario [1,2,3] is one type of nonsingular bounce cosmology [4,5,6,7,8,9], which is often viewed as an important alternative to the standard inflationary paradigm [10,11,12,13]. Comparing with inflation where the primordial fluctuations become frozen at the moment of the Hubble exit, those primordial fluctuations on matter fields in bounce cosmology would continue to increase after the Hubble exit during the contracting phase until the universe arrive at the bouncing phase [9,20], and the contracting phase would yield a different initial condition for the PBH formation and evolution Once these PBHs have formed, the contraction of spacetime could compress and enlarge the primordial matter density, change the PBH horizon radius which can lead to effects on their evolution.
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