The DOI matches its Crossref record; 11 of the 11 references it cites were found in a registry or an index.
Nucleosynthesis Without Computer
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At about 1 second (T ∼ 0.8 MeV), the proton↔neutron reaction rate has slowed relative to expansion such that the proton-to-neutron ratio freezes out.
“However, at about 1 second ( T ∼ 0 . 8 MeV ) the reaction rate has slowed relative to the expansion such that the proton to neutron ratio freezes out.”
From Under an iron sky: On the entropy at the start of the Universe (2021) · cites this paper as Mukhanov (2004)
In our Universe, the abundances of nuclear species can differ significantly from NSE.
“In our Universe, once freeze-out occurs at T ≈ 0 . 84 MeV = 9 . 7 × 10 9 K (Mukhanov, 2004), the abundances of nuclear species can differ significantly from NSE.”
From Under an iron sky: On the entropy at the start of the Universe (2021) · cites this paper as Mukhanov (2004)
In our Universe, freeze-out occurs at T ≈ 0.84 MeV = 9.7 × 10^9 K.
“In our Universe, once freeze-out occurs at T ≈ 0 . 84 MeV = 9 . 7 × 10 9 K (Mukhanov, 2004), the abundances of nuclear species can differ significantly from NSE.”
From Under an iron sky: On the entropy at the start of the Universe (2021) · cites this paper as Mukhanov (2004)
By about 1000 seconds, the Universe has expanded and cooled to the point that nucleosynthesis is over, leaving the baryonic component in the form of hydrogen and helium, with a trace of heavier elements.
“By ∼ 1000 seconds, the Universe has expanded and cooled to the point that nucleosynthesis is over, leaving the baryonic component in the form of hydrogen and helium, with a trace of heavier elements.”
From Under an iron sky: On the entropy at the start of the Universe (2021) · cites this paper as Mukhanov (2004)
After freeze-out, nucleosynthesis begins in earnest at about 100 seconds.
“After this, nucleosynthesis begins in earnest about at ∼ 100 seconds.”
From Under an iron sky: On the entropy at the start of the Universe (2021) · cites this paper as Mukhanov (2004)
Citations
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Flagged first, then by citations
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Cited by
Sorted by citations
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Primordial nucleosynthesis: From precision cosmology to fundamental physics
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Cosmological bounds on pseudo Nambu-Goldstone bosons
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“mple BBN code5 in Mathematica to compute the primordial abundances of D, 3He, 4He, 7Li and 7Be. We have used the minimal reaction network relevant for η ∼ ηCMB and Neff ∼ 3 as detailed for instance in [24, 25, 27]. This allows us to easily compute the outcome of BBN when ALPs have a non trivial role during BBN itself,…”
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Hardy, E., Lasenby, R., March-Russell, J., & West, S. M. (2015) · Journal of High Energy Physics · doi:10.1007/jhep06(2015)011 · Cited by 131
“ucient to make the rate of production of energetically favoured A12 nuclei comparable to the Hubble rate, and so we freeze out with quasi-equilibrium abundances (for a textbook discussion see e.g., [56]). Note that this kind of bottleneck, involving a wrong-sign binding energy dierence rather than merely a small right…”
BackgroundBambi, C., Giannotti, M., & Villante, F. L. (2005) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.71.123524 · Cited by 120
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D’Eramo, F., Fernandez, N., & Profumo, S. (2017) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2017/05/012 · Cited by 140
BBN for the LHC: Constraints on lifetimes of the Higgs portal scalars
Fradette, A., & Pospelov, M. (2017) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.96.075033 · Cited by 107
A survey of dark matter and related topics in cosmology
Young, B.-L. (2016) · Frontiers of Physics · doi:10.1007/s11467-016-0583-4 · Cited by 99
Resonant destruction as a possible solution to the cosmological lithium problem
Chakraborty, N., Fields, B. D., & Olive, K. A. (2011) · Physical review. D. Particles, fields, gravitation, and cosmology/Physical review. D. Particles and fields · doi:10.1103/physrevd.83.063006 · Cited by 74
The hubble tension as a hint of leptogenesis and neutrino mass generation
Escudero, M., & Witte, S. J. (2021) · The European Physical Journal C · doi:10.1140/epjc/s10052-021-09276-5 · Cited by 75
Cosmological signatures of a mirror twin Higgs
Chacko, Z., Curtin, D., Geller, M., & Tsai, Y. (2018) · Journal of High Energy Physics · doi:10.1007/jhep09(2018)163 · Cited by 74
“1 BBN in the SM We first review a simple estimate of the helium fraction in the SM, following closely the analytical procedure of [77] (see also e.”
MethodLuzio, L. D., Gröber, R., Kamenik, J. F., & Nardecchia, M. (2015) · Journal of High Energy Physics · doi:10.1007/jhep07(2015)074 · Cited by 73
Constraints on supersymmetric models from catalytic primordial nucleosynthesis of beryllium
Pospelov, M., Pradler, J., & Steffen, F. D. (2008) · Journal of Cosmology and Astroparticle Physics · doi:10.1088/1475-7516/2008/11/020 · Cited by 64
Giovanetti, C., Lisanti, M., Liu, H., & Ruderman, J. T. (2022) · Physical Review Letters · doi:10.1103/physrevlett.129.021302 · Cited by 58
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Bansal, S., Kim, J. H., Kolda, C., Low, M., & Tsai, Y. (2022) · Journal of High Energy Physics · doi:10.1007/jhep05(2022)050 · Cited by 47
Escudero, M., Ibarra, A., & Maura, V. (2023) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.107.035024 · Cited by 46
“We, however, note that in the few cosmological settings that feature ∆Neff 0, notably MeVscale reheating [63, 64] and scenarios with MeV-scale electrophilic particles [65, 66], these models actually lead to a higher YP, see [67, 68] and would thus enhance the tension with the EMPRESS measurement.”
BackgroundInfluentialPrimordial Nucleosynthesis with Varying Fundamental Constants: A Semianalytical Approach
Landau, S. J., MOSQUERA, M. E., & Vucetich, H. (2006) · The Astrophysical Journal · doi:10.1086/431417 · Cited by 44
“The prediction of the light elements abundances ((4)He, (2)D, (7)Li) produced during the first minutes of the universe can be calculated using numerical (Sarkar) and analytical (Esmailzadeh et al. 1991; Mukhanov 2003) methods.”
MethodCosmological constraints on first-order phase transitions
Yang Bai, A., & Korwar, M. (2022) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.105.095015 · Cited by 45
Dark sector equilibration during nucleosynthesis
Berlin, A., Blinov, N., & Li, S. W. (2019) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.100.015038 · Cited by 44
“These reaction rates are slow compared to Hubble expansion until nD/(np + nn) ∼ O(10−4) [41].”
BackgroundBounds on neutrino-scalar nonstandard interactions from big bang nucleosynthesis
Venzor, J., Pérez-Lorenzana, A., & De-Santiago, J. (2021) · Physical review. D/Physical review. D. · doi:10.1103/physrevd.103.043534 · Cited by 49
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“k data [12]. The bottleneck opens when the rate of conversion of deuterium into heavier elements becomes comparable to the expansion of the universe. This occurs when its abundance reaches X D˘2 10 5 [36]. At this moment, the deuterium burning is still much slower than the reaction n+ p$D+ maintaining deuterium in equ…”
BackgroundInfluentialSynergy between cosmological and laboratory searches in neutrino physics
Gerbino, M., Grohs, E., Lattanzi, M., Abazajian, K. N., Blinov, N., Brinckmann, T., Chen, M., Djurčić, Z., Du, P., Escudero, M., et al. (2023) · Physics of the Dark Universe · doi:10.1016/j.dark.2023.101333 · Cited by 33
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“1, begin with a brief review of the standard BBN analysis, following the discussion in [41].”
BackgroundConstraining the primordial black hole abundance through big-bang nucleosynthesis
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“33), which becomes more efficient since an enhanced abundance of D increases the number of neutrons n at the relevant times [130]; cf.”
BackgroundBig-bang nucleosynthesis and WIMP dark matter in modified gravity
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“re 0(Q) = Z Q 1 dqq(q Q)2(q2 1)1=2: (4.7) The temperature of the mirror sector at which the mirror deuterium bottleneck is crossed is TB DBB ˇ(B DB=B DA)T A DB A , where T A DB is taken as 0.08 MeV [82]. This takes place at a time t DB B = 0:301g 1=2 ? m Plr 2 T =(TB DB )2, meaning that the ratio of mirror protons and…”
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“[32, Section 24], [33, Chapter 4], [34, Chapters 1,4], and [35].”
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“[17–21] and Ref.”
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“…at an initial temperature 42 T ′ = 1 MeV, and evolve the abundances of elements other than ¯ p with the following simplified nuclear reaction network [130]: where we have defined the dimensionless quantity which quantifies the efficiency of nuclear reactions on the timescale of fireball expansion.”
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“The rates γ nν → pe and γ ne + → p ¯ ν can be found, e.g., in [30].”
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“6 MeV in standard cosmology [76, 77, 78, 79, 80, 81].”
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“Thus, while modern computer codes (e.g. Giovanetti et al. 2025, and references therein) perform full calculations of all the relevant reactions, the main channels are fewer and lend themselves to be modelled analytically (Mukhanov 2004).”
Origin of the Universe and Planetary Systems
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“Following Mukhanov (2004) we take a non-equilibrium freeze-out ratio of neutron number density (nn) to baryon number density (nN): nn nN (Tf) = ∫ ∞ 0 exp [ −5.42(π2 30 g∗(Tf )) − 1 2 ∫ y 0 (x+ 1 4 )2(1 + e− 1 x )dx ] 2y2(1 + cosh(1/y)) dy, (3) where y = kTf/Q.”
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“As shown by Mukhanov [27], the relative number density of neutrons is given by an asymptotic series of the form,”
BackgroundMethodInfluentialBBN-simple: How to bake a universe-sized cake
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“Theoretical treatments in textbooks [19, 45] and the “no computer” calculations [46, 47] do produce reasonably accurate results, but seem too technical and equation-heavy to be reasonably covered in a graduate course or a homework assignment.”
Ghosh, D. (2024) · The European Physical Journal C · doi:10.1140/epjc/s10052-024-12963-8 · Cited by 2
“In passing, we note that the accidental stability of χ may be ensured if there is an exact cancellation between diagrams coming from other possible interactions of χ , e.g. similar loops with mesons.”
BackgroundLight scalar dark matter coupled to a trace of energy-momentum tensor
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Ghosh, S., Boddy, K. K., & Yu, T. (2026) · Physical review. D/Physical review. D. · doi:10.1103/pbgn-1mts · Cited by 1
Thermal damping of mass-modulating scalars
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From Primordial4He Abundance to the Higgs Field
Gaßner, J. M., Lesch, H., & Arenhövel, H. (2008) · The Astrophysical Journal · doi:10.1086/591039 · Cited by 1
“Hence, we have to derive nonequilibrium concentrations, where we follow the example calculations of Mukhanov (2004).”
BackgroundConsistent N eff fitting in big bang nucleosynthesis analysis
Ganguly, S., Jung, T. H., & Yun, S. (2026) · Physical review. D/Physical review. D. · doi:10.1103/46fz-9wqk
Metadata
- Authors
- Mukhanov, V.
- Affiliations
- Ludwig-Maximilians-Universität München (DE)
- Corresponding author
- Mukhanov, V.
- ORCID
- Mukhanov, V.
- Venue
- International Journal of Theoretical Physics
- Published
- 2004-03
- Volume
- 43
- Issue
- 3
- Pages
- 669-693
- ISSN
- 0020-7748 (ISSN-L)
- 1572-9575
- OpenAlex
- W2062766322
- Cited by
- 55
- References
- 11
- Citations by year
- 2026: 6 · 2025: 6 · 2024: 3 · 2023: 5 · 2022: 4 · 2021: 4 · 2020: 3 · 2019: 1 · 2018: 1 · 2017: 2 · 2016: 3 · 2015: 2 · 2012: 1
- FWCI
- 0.59
- Type
- journal article
- Language
- en
- Open access
- green
- arxiv.org
- Licence
- Locations
- International Journal of Theoretical Physics (publishedVersion)
- arXiv (Cornell University) (submittedVersion)
- arXiv (Cornell University)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Cosmology and Gravitation Theories
- Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Nuclear physics research studies
- Physical Sciences › Physics and Astronomy › Nuclear and High Energy Physics › Neutrino Physics Research
- Keywords
- big bang nucleosynthesis, light element abundances, analytical derivation, early universe, helium-4, deuterium, lithium-7, beryllium-7
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