Primordial black holes and the origin of the matter–antimatter asymmetry

García-Bellido, J.

doi:10.1098/rsta.2019.0091

Cited by 15 publications

(18 citation statements)

References 64 publications

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“…In either case, it has been found that a PBHs mass spectrum spanning a few orders of magnitude in the range of O(0.01 − 1000) which for any particular mass does not reach more than 40% of the DM energy density is still viable (see in [15,20,36,70,71]).…”

Section: Observational Constraintsmentioning

confidence: 99%

The Clustering Dynamics of Primordial Black Holes in N-Body Simulations

2021

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We explore the possibility that Dark Matter (DM) may be explained by a nonuniform background of approximately stellar mass clusters of Primordial Black Holes (PBHs) by simulating the evolution from recombination to the present with over 5000 realisations using a Newtonian N-body code. We compute the cluster rate of evaporation and extract the binary and merged sub-populations along with their parent and merger tree histories, lifetimes and formation rates, the dynamical and orbital parameter profiles, the degree of mass segregation and dynamical friction and power spectrum of close encounters. Overall, we find that PBHs can constitute a viable DM candidate, and that their clustering presents a rich phenomenology throughout the history of the Universe. We show that binary systems constitute about 9.5% of all PBHs at present, with mass ratios of q¯B=0.154, and total masses of m¯T,B=303M⊙. Merged PBHs are rare, about 0.0023% of all PBHs at present, with mass ratios of q¯B=0.965 with total and chirp masses of m¯T,B=1670M⊙ and m¯c,M=642M⊙, respectively. We find that cluster puffing up and evaporation leads to bubbles of these PBHs of order 1 kpc containing at present times about 36% of objects and mass, with one-hundred pc-sized cores. We also find that these PBH sub-haloes are distributed in wider PBH haloes of order hundreds of kpc, containing about 63% of objects and mass, coinciding with the sizes of galactic halos. We find at last high rates of close encounters of massive Black Holes (M∼1000M⊙), with ΓS=(1.2+5.9−0.9)×107yr−1Gpc−3 and mergers with ΓM=1337±41yr−1Gpc−3.

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Section: Observational Constraintsmentioning

confidence: 99%

The Clustering Dynamics of Primordial Black Holes in N-Body Simulations

2021

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“…In either case it has been found that a PBHs mass spectrum spanning a few orders of magnitude in the range of O(0.01 − 1000) which for any particular mass does not reach more than 40% of the DM energy density is still viable (see Refs. [15,20,35,69,70]).…”

Section: B Observational Constraintsmentioning

confidence: 99%

The clustering dynamics of primordial black boles in $N$-body simulations

Trashorras,

García-Bellido,

Nesseris

2020

Preprint

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We explore the possibility that Dark Matter (DM) may be explained by a non-uniform background of approximately stellar-mass clusters of Primordial Black Holes (PBHs), by simulating the evolution them from recombination to the present with over 5000 realisations using a Newtonian N -body code. We compute the cluster rate of evaporation, and extract the binary and merged sub-populations along with their parent and merger tree histories, lifetimes and formation rates; the dynamical and orbital parameter profiles, the degree of mass segregation and dynamical friction, and power spectrum of close encounters. Overall, we find that PBHs can constitute a viable DM candidate, and that their clustering presents a rich phenomenology throughout the history of the Universe. We show that binary systems constitute about 9.5% of all PBHs at present, with mass ratios of qB = 0.154, and total masses of mT,B = 303 M . Merged PBHs are rare, about 0.0023% of all PBHs at present, with mass ratios of qM = 0.965 with total and chirp masses of mT,M = 1670 M and mc,M = 642 M respectively. We find that cluster puffing up and evaporation leads to bubbles of these PBHs of order 1 kpc containing at present times about 36% of objects and mass, with hundred pc sized cores. We also find that these PBH sub-haloes are distributed in wider PBH haloes of order hundreds of kpc, containing about 63% of objects and mass, coinciding with the sizes of galactic halos. We find at last high rates of close encounters of massive Black Holes (M ∼ 1000 M ), with Γ S = (1.2 +5.9 −0.9 ) × 10 7 yr −1 Gpc −3 and mergers with Γ M = 1337 ± 41 yr −1 Gpc −3 .

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“…Following the predictions in [1] I make the simplifying assumption that all dark matter exists in the form of 1.4 M black holes, created seconds after the Big Bang. As we will see, for most of the cosmic history these black holes move at supersonic speeds among the baryons and will therefore undergo Bondi-Hoyle-Lyttleton quasi-spherical accretion [30][31][32].…”

Section: Basic Parameters Of the Toy Modelmentioning

confidence: 99%

“…In a recently published theoretical prediction [1,9] PBH are created in the QCD phase transitions (around 100 MeV) of different particle families freezing out of the primordial Quark-gluon plasma within the first two seconds after the inflationary phase. When W +/− , Z bosons, baryons, pions are created, and e + e − pairs annihilate, they leave an imprint in form of a significant reduction of the sound speed at the corresponding phase transitions, and allow regions of high curvature to collapse and form PBH.…”

Section: Introductionmentioning

confidence: 99%

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Illuminating the dark ages: Cosmic backgrounds from accretion onto primordial black hole dark matter

Hasinger

2020

Preprint

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The recent interpretation of cold dark matter as the sum of contributions of different mass Primordial Black Hole (PBH) families [1] could explain a number of so far unsolved mysteries, like e.g. the massive seed black holes required to create the supermassive black holes in the earliest QSOs, the ubiquitous massive LIGO/VIRGO massive binary black holes, or even the putative "Planet X" PBH in our Solar System. By far the most abundant family of PBH should be around the Chandrasekhar mass (1.4 M ). This prediction may already have been vindicated by the recent OGLE/GAIA discovery of a sizeable population of putative black holes in the mass range 1-10 M .Here I assume that all dark matter exists in the form of 1.4 M PBH and estimate the contribution of baryon accretion onto this population to various cosmic background radiations, concentrating first on the cross-correlation signal between the Cosmic X-ray and the Cosmic infrared background fluctuations discovered in deep Chandra and Spitzer surveys. I assume Bondi accretion with reasonable parameters like baryon density and the effective relative velocity between baryons and PBH as well as appropriate accretion and radiation efficiencies and integrate these over cosmic time. I indeed predict a contribution of PBH accretion to the X-ray background consistent with the residual X-ray fluctuation signal. This signal peaks at redshifts z≈17-30, consistent with other constraints requiring the signal to come from such high redshifts. The PBH contribution to the 2-5 µm Cosmic Infrared background fluctuations is only about 1%, so that these likely come from star formation processes in regions associated with the PBH.I discuss a number of other phenomena, which could be significantly affected by the PBH accretion. Magnetic fields are an essential ingredient in the Bondi accretion process, and argue that the PBH can play an important role in amplifying magnetic seed fields in the early universe and maintaining them until the galactic dynamo processes set in. Next I study the contribution of the assumed PBH population to the re-ionization history of the universe and find that they do not conflict with the stringent ionization limits set by the most recent Planck measurements. X-ray heating from the PBH population can provide a contribution to the entropy floor observed in groups of galaxies. The tantalizing redshifted 21-cm absorption line feature observed by em EDGES could be connected to the radio emission contributed by PBH to the cosmic background radiation. Finally, the diffuse X-ray emission in the Galactic Center region is not violated by the assumed PBH dark matter, on the contrary, some of the discrete sources resolved in the deepest Chandra observations of the Galactic Ridge could indeed be accreting PBH. Contents 1 Introduction 1 2 Basic parameters of the toy model 3 3 Accretion spectrum and radiative efficiency 6 4 The contribution of PBH to the extragalactic background light 8 5 Discussion 11 5.1 Linear versus post-linear growth 11 5.2 Magnetic fields in the early...

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Primordial black holes and the origin of the matter–antimatter asymmetry

Cited by 15 publications

References 64 publications

The Clustering Dynamics of Primordial Black Holes in N-Body Simulations

The Clustering Dynamics of Primordial Black Holes in N-Body Simulations

The clustering dynamics of primordial black boles in $N$-body simulations

Illuminating the dark ages: Cosmic backgrounds from accretion onto primordial black hole dark matter

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