Publisher’s Note: The<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow /><mml:mrow><mml:mn>3</mml:mn></mml:mrow></mml:msup></mml:mrow><mml:mi mathvariant="normal">He</mml:mi><mml:mo>(</mml:mo><mml:mrow><mml:mrow><mml:mover><mml:mrow><mml:mi>d</mml:mi></mml:mrow><mml:mrow><mml:mo>→</mml:mo></mml:mrow></mml:mover></mml:mrow></mml:mrow><mml:mrow><mml:msup><mml:mrow><mml:mo>,</mml:mo><mml:mi>p</mml:mi><mml:mo>)</mml:mo></mml:mrow><mml:mrow><mml:mn>4</mml:mn

Geist, W. H.; Brune, C. R.; Karwowski, H. J.; Ludwig, E. J.; Veal, K. D.; Hale, G. M.

doi:10.1103/physrevc.67.059904

Cited by 6 publications

(6 citation statements)

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“…There has been a large number of recent works [100,131,156,80,157,159,71,160,161,162,163,164,165,166,167,168, dealing with experimental measurements, theoretical calculations, and the determination of uncertainties of the cross sections listed in Eqs. (21-2.4).…”

Section: Bbn Of Elements Up To Berylliummentioning

confidence: 99%

Frontiers in nuclear astrophysics

Bertulani

Kajino

2016

Progress in Particle and Nuclear Physics

107

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The synthesis of nuclei in diverse cosmic scenarios is reviewed, with a summary of the basic concepts involved before a discussion of the current status in each case is made. We review the physics of the early universe, the proton to neutron ratio influence in the observed helium abundance, reaction networks, the formation of elements up to beryllium, the inhomogeneous Big Bang model, and the Big Bang nucleosynthesis constraints on cosmological models. Attention is paid to element production in stars, together with the details of the pp chain, the pp reaction, 3 He formation and destruction, electron capture on 7 Be, the importance of 8 B formation and its relation to solar neutrinos, and neutrino oscillations. Nucleosynthesis in massive stars is also reviewed, with focus on the CNO cycle and its hot companion cycle, the rp-process, triple-α capture, and red giants and AGB stars. The stellar burning of carbon, neon, oxygen, and silicon is presented in a separate section, as well as the slow and rapid nucleon capture processes and the importance of medium modifications due to electrons also for pycnonuclear reactions. The nucleosynthesis in cataclysmic events such as in novae, X-ray bursters and in core-collapse supernovae, the role of neutrinos, and the supernova radioactivity and light-curve is further discussed, as well as the structure of neutron stars and its equation of state. A brief review of the element composition found in cosmic rays is made in the end.

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Section: Bbn Of Elements Up To Berylliummentioning

confidence: 99%

Frontiers in nuclear astrophysics

Bertulani

Kajino

2016

Progress in Particle and Nuclear Physics

107

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“…Since it is responsible for destroying 3 He before it can capture an α particle to form 7 Be, the primordial Li abundance is anti-correlated with the 3 He(d, p)α cross section in the BBN energy range from circa 60-360 keV. The polynomial fit of Cyburt (2004) to the data of Bonner et al (1952); Kunz (1955); Zhichang et al (1977); Möller & Besenbacher (1980); Krauss et al (1987) and Geist et al (2000) resulted in a 6.6% rate uncertainty, translating into a 5.0% uncertainty in primordial 7 Li/H.…”

Section: Resultsmentioning

confidence: 99%

Measurements of Nuclear Reactions that Create and Destroy Li and Be during BBN

Davids

2020

Preprint

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I review measurements of the most important reactions involved in the creation and destruction of Li and Be during big bang nucleosynthesis (BBN) as well as their uncertainties and the relative contributions they make to the uncertainty in the primordial 7 Li abundance ( 7 Li/H). Examining the sensitivity of calculated 7 Li/H to these reactions as predicted by different BBN codes I find no significant differences. I compare my calculation of primordial 7 Li/H to some recently published values and conclude that in the absence of a major undetected experimental blunder, nuclear physics uncertainties cannot account for the cosmological Li problem. With an estimated 13% uncertainty in the calculated abundance, the discrepancy with observation amounts to some 4.6σ.

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“…3 He (d , p) 4 He This reaction is not included in NACRE, but is present in CF88. The experimental data sets adopted here are KR87a [80], SC89 [120], GE99 [121], CO00 [122], AL01 [123], and LA05 [124] † , covering the 0.005 < ∼ E cm < ∼ 1 MeV range. [125,126] are superseded by AL01.…”

Section: LImentioning

confidence: 99%

NACRE II: an update of the NACRE compilation of charged-particle-induced thermonuclear reaction rates for nuclei with mass number $A < 16$

Xu,

Takahashi,

Goriely

et al. 2013

Preprint

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An update of the NACRE compilation [Angulo et al., Nucl. Phys. A 656 (1999) 3] is presented. This new compilation, referred to as NACRE II, reports thermonuclear reaction rates for 34 charged-particle induced, two-body exoergic reactions on nuclides with mass number A < 16, of which fifteen are particle-transfer reactions and the rest radiative capture reactions. When compared with NACRE, NACRE II features in particular (1) the addition to the experimental data collected in NACRE of those reported later, preferentially in the major journals of the field by early 2013, and (2) the adoption of potential models as the primary tool for extrapolation to very low energies of astrophysical S-factors, with a systematic evaluation of uncertainties.As in NACRE, the rates are presented in tabular form for temperatures in the 10 6 < ∼ T ≤ 10 10 K range. Along with the 'adopted' rates, their low and high limits are provided. The new rates are available in electronic form as part of the Brussels Library (BRUSLIB) of nuclear data. The NACRE II rates also supersede the previous NACRE rates in the Nuclear Network Generator (NETGEN) for astrophysics.[http://www.astro.ulb.ac.be/databases.html.]

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Publisher’s Note: The3He(d→,p)4

Cited by 6 publications

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Frontiers in nuclear astrophysics

Frontiers in nuclear astrophysics

Measurements of Nuclear Reactions that Create and Destroy Li and Be during BBN

NACRE II: an update of the NACRE compilation of charged-particle-induced thermonuclear reaction rates for nuclei with mass number $A < 16$

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