The baryon density of the Universe from an improved rate of deuterium burning

Mossa, V.; Stöckel, K.; Cavanna, F.; Ferraro, F.; Aliotta, M.; Barile, F.; Bemmerer, D.; Best, A.; Boeltzig, A.; Broggini, C.; Bruno, Carlo; Caciolli, A.; Chillery, T.; Ciani, G. F.; Corvisiero, P.; Csedreki, L.; Davinson, T.; Depalo, R.; Leva, A. Di; Elekes, Z.; Fiore, E. M.; Formicola, A.; Fülöp, Zs.; Gervino, G.; Guglielmetti, A.; Gustavino, C.; Gyürky, Gy.; Imbriani, G.; Junker, M.; Kievsky, A.; Kochanek, I.; Lugaro, Maria; Marcucci, L. E.; Mangano, G.; Marigo, Paola; Masha, E.; Menegazzo, R.; Pantaleo, F. R.; Paticchio, V.; Perrino, R.; Piatti, D.; Pisanti, O.; Prati, P.; Schiavulli, L.; Straniero, O.; Szücs, T.; Takács, M. P.; Trezzi, D.; Viviani, M.; Zavatarelli, S.

doi:10.1038/s41586-020-2878-4

Cited by 153 publications

(267 citation statements)

References 37 publications

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“…On the other hand, the deuterium abundance is strongly dependent upon the baryon energy density while only moderately dependent upon the expansion rate, potentially modified by N eff . Importantly, although the recent results from the LUNA collaboration [155] have reduced the theoretical prediction for deuterium, it is still at the ∼ 2.8% level [156] -see also [157] and [158] which report 1.5 and 4.4% uncertainties, respectively. In order to understand the effect of these constraints in our parameter space we have used the predictions and theoretical uncertainties from the recent analysis of [156].…”

Section: Appendix C: Big Bang Nucleosynthesismentioning

confidence: 95%

The hubble tension as a hint of leptogenesis and neutrino mass generation

Escudero

Witte

2021

Eur. Phys. J. C

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The majoron, a neutrinophilic pseudo-Goldstone boson conventionally arising in the context of neutrino mass models, can damp neutrino free-streaming and inject additional energy density into neutrinos prior to recombination. The combination of these effects for an eV-scale mass majoron has been shown to ameliorate the outstanding $$H_0$$ H 0 tension, however only if one introduces additional dark radiation at the level of $$\Delta N_{\mathrm{eff}} \sim 0.5$$ Δ N eff ∼ 0.5 . We show here that models of low-scale leptogenesis can naturally source this dark radiation by generating a primordial population of majorons from the decays of GeV-scale sterile neutrinos in the early Universe. Using a posterior predictive distribution conditioned on Planck2018+BAO data, we show that the value of $$H_0$$ H 0 observed by the SH$$_0$$ 0 ES collaboration is expected to occur at the level of $$\sim 10\%$$ ∼ 10 % in the primordial majoron cosmology (to be compared with $$\sim 0.1\%$$ ∼ 0.1 % in the case of $$\Lambda $$ Λ CDM). This insight provides an intriguing connection between the neutrino mass mechanism, the baryon asymmetry of the Universe, and the discrepant measurements of $$H_0$$ H 0 .

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Section: Appendix C: Big Bang Nucleosynthesismentioning

confidence: 95%

The hubble tension as a hint of leptogenesis and neutrino mass generation

Escudero

Witte

2021

Eur. Phys. J. C

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“…The duration of the D-burning phase in pre-MS depends not only on the stellar mass but it is also proportional to the original stellar deuterium mass fraction abundance. Observations suggest that for disc stars a value of X D ≈ 2 × 10 − 5 should be adopted (see e.g., the review by Sembach, 2010); such a value is smaller than that predicted by the BBN (X D ≈ 4 × 10 − 5 , see e.g., Steigman et al, 2007;Pettini et al, 2008;Pitrou et al, 2018;Mossa et al, 2020), as expectede.g., by galactic evolution modelsbecause deuterium is destroyed in stars.…”

Section: General Characteristics Of Standard Pre-main Sequence Evolutionmentioning

confidence: 80%

“…Adelberger et al (2011) redetermined the best value for the astrophysical factor S(E) for such a reaction at zero energy [S(0)] and the uncertainty on it, concluding that the current uncertainty on S(0) for such burning reaction is ≈ 7%. Recently, Mossa et al (2020) redetermined the D+p cross sections at energies typical of the BBN (between 32-263 KeV)thus larger than those used in stellar calculationsestimating an uncertainty of about 3%.…”

Section: Effects Of Deuterium Burning Cross Sections On Pre-ms Evolutionmentioning

confidence: 99%

Theoretical Predictions of Surface Light Element Abundances in Protostellar and Pre-Main Sequence Phase

Tognelli

Degl’Innocenti

Moroni

et al. 2021

Front. Astron. Space Sci.

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Theoretical prediction of surface stellar abundances of light elements–lithium, beryllium, and boron–represents one of the most interesting open problems in astrophysics. As well known, several measurements of 7Li abundances in stellar atmospheres point out a disagreement between predictions and observations in different stellar evolutionary phases, rising doubts about the capability of present stellar models to precisely reproduce stellar envelope characteristics. The problem takes different aspects in the various evolutionary phases; the present analysis is restricted to protostellar and pre-Main Sequence phases. Light elements are burned at relatively low temperatures (T from ≈2 to ≈5 million degrees) and thus in the early evolutionary stages of a star they are gradually destroyed at different depths of stellar interior mainly by (p, α) burning reactions, in dependence on the stellar mass. Their surface abundances are strongly influenced by the nuclear cross sections, as well as by the extension toward the stellar interior of the convective envelope and by the temperature at its bottom, which depend on the characteristics of the star (mass and chemical composition) as well as on the energy transport in the convective stellar envelope. In recent years, a great effort has been made to improve the precision of light element burning cross sections. However, theoretical predictions surface light element abundance are challenging because they are also influenced by the uncertainties in the input physics adopted in the calculations as well as the efficiency of several standard and non-standard physical processes active in young stars (i.e. diffusion, radiative levitation, magnetic fields, rotation). Moreover, it is still not completely clear how much the previous protostellar evolution affects the pre-Main Sequence characteristics and thus the light element depletion. This paper presents the state-of-the-art of theoretical predictions for protostars and pre-Main Sequence stars and their light element surface abundances, discussing the role of (p, α) nuclear reaction rates and other input physics on the stellar evolution and on the temporal evolution of the predicted surface abundances.

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“…The 2 H(p, γ ) 3 He reaction has been studied previously in experiments using a proton beam irradiating frozen heavy water targets [11][12][13][14][15], a windowless gas target deep underground [16,17], or deuterated titanium targets [18]. Recently, 2 H(p, γ ) 3 He data have also been reported from an experiment using an inertially confined plasma of hydrogen and deuterium [19].…”

Section: Introductionmentioning

confidence: 99%

“…The symbols correspond to the experimental data of studies past 1990 by Refs. [13][14][15][16][17][18][19]. The solar fusion II [21] fit curve is shown in black.…”

Section: Introductionmentioning

confidence: 99%

Measurement of theH2(p,γ)He3S
Turkat
¹
,
Hammer
²
,
Masha
³

et al. 2021
Phys. Rev. C
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0
20
0
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Recent astronomical data have provided the primordial deuterium abundance with percent precision. As a result, big bang nucleosynthesis may provide a constraint on the universal baryon to photon ratio that is as precise as, but independent from, analyses of the cosmic microwave background. However, such a constraint requires that the nuclear reaction rates governing the production and destruction of primordial deuterium are sufficiently well known. Here, a new measurement of the 2 H(p, γ ) 3 He cross-section is reported. This nuclear reaction dominates the error on the predicted big bang deuterium abundance. A proton beam of 400-1650 keV beam energy was incident on solid titanium deuteride targets, and the emitted γ rays were detected in two high-purity germanium detectors at angles of 55 • and 90 • , respectively. The deuterium content of the targets has been obtained in situ by the 2 H( 3 He, p) 4 He reaction and offline using the elastic recoil detection method. The astrophysical S factor has been determined at center of mass energies between 265 and 1094 keV, addressing the uppermost part of the relevant energy range for big bang nucleosynthesis and complementary to ongoing work at lower energies. The new data support a higher S factor at big bang temperatures than previously assumed, reducing the predicted deuterium abundance.

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The baryon density of the Universe from an improved rate of deuterium burning

Cited by 153 publications

References 37 publications

The hubble tension as a hint of leptogenesis and neutrino mass generation

The hubble tension as a hint of leptogenesis and neutrino mass generation

Theoretical Predictions of Surface Light Element Abundances in Protostellar and Pre-Main Sequence Phase

Measurement of theH2(p,γ)He3S
Turkat
¹
,
Hammer
²
,
Masha
³

et al. 2021
Phys. Rev. C
Self Cite
7
0
20
0
View full text Add to dashboard Cite

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The baryon density of the Universe from an improved rate of deuterium burning

Cited by 153 publications

References 37 publications

The hubble tension as a hint of leptogenesis and neutrino mass generation

The hubble tension as a hint of leptogenesis and neutrino mass generation

Theoretical Predictions of Surface Light Element Abundances in Protostellar and Pre-Main Sequence Phase

Measurement of theH2(p,γ)He3STurkat1, Hammer2, Masha3 et al. 2021Phys. Rev. CSelf Cite70200View full textAdd to dashboardCite

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Measurement of theH2(p,γ)He3S
Turkat
¹
,
Hammer
²
,
Masha
³

et al. 2021
Phys. Rev. C
Self Cite
7
0
20
0
View full text Add to dashboard Cite