<i>sup3</i>He<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:msup><mml:mrow><mml:mo>+</mml:mo></mml:mrow><mml:mrow><mml:mn>3</mml:mn></mml:mrow></mml:msup></mml:mrow></mml:math>He reaction cross sections at 17.9, 21.7, and 24.0 MeV

Brown, Ronald E.; Correll, F. D.; Hegland, P. M.; Koepke, J. A.; Poppe, C. H.

doi:10.1103/physrevc.35.383

Cited by 8 publications

(3 citation statements)

References 15 publications

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“…Our adopted data from Dwarakanath & Winkler (1971 Several data sets that were used in previous evaluations (Angulo et al 1999;Descouvemont et al 2004;Adelberger et al 2011;Xu et al 2013) were not incorporated into our analysis. For example, Brown et al (1987) measured the cross section at energies too high to be of interest here, while Dwarakanath (1974); Bacher & Tombrello (1967); Wang et al (1966) did not provide enough information to reliably estimate the separate contributions of statistical and systematic uncertainties.…”

Section: B a Simple Example: Linear Regressionmentioning

confidence: 97%

Bayesian Estimation of Thermonuclear Reaction Rates

Iliadis

Anderson

Coc

et al. 2016

ApJ

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The problem of estimating non-resonant astrophysical S-factors and thermonuclear reaction rates, based on measured nuclear cross sections, is of major interest for nuclear energy generation, neutrino physics, and element synthesis. Many different methods have been applied in the past to this problem, almost all of them based on traditional statistics. Bayesian methods, on the other hand, are now in widespread use in the physical sciences. In astronomy, for example, Bayesian statistics is applied to the observation of extra-solar planets, gravitational waves, and type Ia supernovae. However, nuclear physics, in particular, has been slow to adopt Bayesian methods. We present astrophysical S-factors and reaction rates based on Bayesian statistics. We develop a framework that incorporates robust parameter estimation, systematic effects, and non-Gaussian uncertainties in a consistent manner. The method is applied to the d(p,γ) 3 He, 3 He( 3 He,2p) 4 He, and 3 He(α,γ) 7 Be reactions, important for deuterium burning, solar neutrinos, and big bang nucleosynthesis.

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Section: B a Simple Example: Linear Regressionmentioning

confidence: 97%

Bayesian Estimation of Thermonuclear Reaction Rates

Iliadis

Anderson

Coc

et al. 2016

ApJ

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“…For the central solar temperature one has E o =22 keV and ∆=12 keV. The available experimental data [91][92][93][94][95][96][97] are shown in Fig. 17.…”

Section: Nuclear Reactions In the Sunmentioning

confidence: 99%

Solar neutrinos: beyond standard solar models

et al. 1997

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After a short survey of the physics of solar neutrinos, giving an overview of hydrogen burning reactions, predictions of standard solar models and results of solar neutrino experiments, we discuss the solar-model-independent indications in favour of non-standard neutrino properties. The experimental results look to be in contradiction with each other, even disregarding some experiment: unless electron neutrinos disappear in their trip from the sun to the earth, the fluxes of intermediate energy neutrinos (those from 7 Be electron capture and from the CNO cycle) result to be unphysically negative, or anyway extremely reduced with respect to standard solar model predictions. Next we review extensively non-standard solar models built as attempts to solve the solar neutrino puzzle. The dependence of the central solar temperature on chemical composition, opacity, age and on the values of the astrophysical S-factors for hydrogen-burning reactions is carefully investigated. Also, possible modifications of the branching among the various pp-chains in view of nuclear physics uncertainties are examined. Assuming standard neutrinos, all solar models examined fail in reconciling theory with experiments, even when the physical and chemical inputs are radically changed with respect to present knowledge and even if some of the experimental results are discarded.

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“…The experimental data sets referred to in NACRE are WA66 [137], BA67 [138], DW71 [139], DW74 [140], BR87b [141], KR87b [142] and JU98 [143], covering the 0.02 < ∼ E cm < ∼ 12 MeV range. [144] was superseded by JU98.…”

Section: Hementioning

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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sup3He+3He reaction cross sections at 17.9, 21.7, and 24.0 MeV

Cited by 8 publications

References 15 publications

Bayesian Estimation of Thermonuclear Reaction Rates

Bayesian Estimation of Thermonuclear Reaction Rates

Solar neutrinos: beyond standard solar models

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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