Big Bang Nucleosynthesis

Grohs, Evan; Fuller, George M.

doi:10.1007/978-981-15-8818-1_127-1

Cited by 4 publications

(7 citation statements)

References 101 publications

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“…(2.14), we may use current BBN constraints [104,246] (see Ref. [247] for a recent review) to place an upper bound on the initial fraction of evaporated PBHs, which reads…”

Section: Peak Frequency (F Peak [Khz])mentioning

confidence: 99%

“…(a) BBN & CMB. BBN predictions [246,247,276,277] as well as CMB observations [216,278] are sensitive to the presence of additional relativistic particles (sometimes also called dark radiation). Constraints from BBN and CMB are then usually parametrized with an effective number 2.…”

Section: Complementary Probesmentioning

confidence: 99%

“…In light blue we plot the upper bounds from the LVK collaboration [275]. The blue dashed line shows the current constraint from BBN [104,246,247].…”

Section: Complementary Probesmentioning

confidence: 99%

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Gravitational wave constraints on the primordial black hole dominated early universe

Domènech

Lin

Sasaki

2021

J. Cosmol. Astropart. Phys.

105

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We calculate the gravitational waves (GWs) induced by the density fluctuations due to the inhomogeneous distribution of primordial black holes (PBHs) in the case where PBHs eventually dominate and reheat the universe by Hawking evaporation. The initial PBH density fluctuations are isocurvature in nature. We find that most of the induced GWs are generated right after evaporation, when the universe transits from the PBH dominated era to the radiation dominated era and the curvature perturbation starts to oscillate wildly. The strongest constraint on the amount of the produced GWs comes from the big bang nucleosynthesis (BBN). We improve previous constraints on the PBH fraction and find that it cannot exceed 10-4. Furthermore, this maximum fraction decreases as the mass increases and reaches 10-12 for MPBH∼ 5×108 g, which is the largest mass allowed by the BBN constraint on the reheating temperature. Considering that PBH may cluster above a given clustering scale, we also derive a lower bound on the scale of clustering. Interestingly, the GW spectrum for MPBH∼ 104 -108 g enters the observational window of LIGO and DECIGO and could be tested in the future. Although we focus on the PBH dominated early universe in this paper, our methodology is applicable to any model with early isocurvature perturbation.

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“…(2.14), we may use current BBN constraints [104,246] (see Ref. [247] for a recent review) to place an upper bound on the initial fraction of evaporated PBHs, which reads…”

Section: Peak Frequency (F Peak [Khz])mentioning

confidence: 99%

Section: Complementary Probesmentioning

confidence: 99%

See 1 more Smart Citation

Gravitational wave constraints on the primordial black hole dominated early universe

Domènech

Lin

Sasaki

2021

J. Cosmol. Astropart. Phys.

105

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“…The aim of this section is not to review all of BBN -we leave this task to excellent reviews such as [28,29] or the works describing the respective codes such as [5,30,31]. Instead, this section aims to give a short description of the most important aspects allowing the reader to quickly develop a physical intuition of how the different parts of BBN work and how the abundances are connected.…”

Section: A Short Theory Summarymentioning

confidence: 99%

The 2024 BBN baryon abundance update

Schöneberg

2024

J. Cosmol. Astropart. Phys.

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We revisit the state of the light element abundances from big bang nucleosynthesis in early 2024 with particular focus on the derived baryon abundance. We find that the largest differences between the final baryon abundances are typically driven by the assumed Deuterium burning rates, characterized in this work by the underlying code. The rates from theoretical ab-initio calculations favor smaller baryon abundances, while experimentally-determined rates prefer higher abundances. Through robust marginalization over a wide range of nuclear rates, the recently released PRyMordial code allows for a conservative estimate of the baryon abundance at Ω bh 2 = 0.02218 ± 0.00055 (using PDG-recommended light element abundances) in ΛCDM and Ω bh 2 = 0.02196 ± 0.00063 when additional ultra-relativistic relics are considered (ΛCDM + N eff). These additional relics themselves are constrained to ΔN eff = -0.10 ± 0.21 by light element abundances alone.

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“…We show the GW spectral density in red in figure 2. From equation (2.14), we may use current BBN constraints [108,257] (see [258] for a recent review) to place an upper bound on the initial fraction of evaporated PBHs, which reads…”

Section: A Gws Associated With Pbh Reheating I (Isocurvature Induced ...mentioning

confidence: 99%

Probing primordial black hole scenarios with terrestrial gravitational wave detectors

Domènech,

Sasaki

2024

Class. Quantum Grav.

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It is possible that primordial black holes constitute (or constituted) a significant fraction of the energy budget of our universe. Terrestrial gravitational wave detectors offer the opportunity to test the existence of primordial black holes in two different mass ranges, from $10^2\,{\rm g}-10^{16}\,{\rm g}$ to $10^{-6}\,M_\odot-100 \,M_\odot$. The first mass window is open via induced gravitational waves, and the second one is by gravitational waves from binary mergers. In this review, we outline and explain the different gravitational wave signatures of primordial black holes that may be probed by terrestrial gravitational wave detectors, such as the current LIGO/Virgo/KAGRA and future ones like Einstein Telescope and Cosmic Explorer. We mainly focus on the associated GW background signals and provide rough estimates for their typical frequency and amplitude. We also discuss complementary probes for these primordial black hole mass ranges.

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Big Bang Nucleosynthesis

Cited by 4 publications

References 101 publications

Gravitational wave constraints on the primordial black hole dominated early universe

Gravitational wave constraints on the primordial black hole dominated early universe

The 2024 BBN baryon abundance update

Probing primordial black hole scenarios with terrestrial gravitational wave detectors

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