A compilation of charged-particle induced thermonuclear reaction rates

Angulo, C.; Arnould, M.; Rayet, M.; Descouvemont, Pierre; Baye, Daniel Jean; Leclercq‐Willain, Ch.; Coc, A.; Barhoumi, S.; Aguer, P.; Rolfs, C.; Kunz, R.; Hammer, J. W.; Mayer, A.; Paradellis, T.; Kossionides, S.; Chronidou, C.; Spyrou, Konstantinos; Degl’Innocenti, S.; Fiorentini, G. A.; Ricci, B.; Zavatarelli, S.; Providência, C.; Wolters, H.; Soares, J.C.; Grama, C.; Rahighi, J.; Shotter, A.C.; Rachti, M. Lamehi

doi:10.1016/s0375-9474(99)00030-5

Cited by 2,094 publications

(1,670 citation statements)

References 525 publications

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“…The thermonuclear reaction rate obtained based on our data is much lower than the previous rate by Caughlan and Fowler (CF88, [28] ) but also lower than all other previously reported thermonuclear reaction rates [15,27,29] (see Fig. 6 and Table 4 ).…”

Section: Thermonuclear Reaction Rate and Astrophysical Implicationscontrasting

confidence: 74%

Big Bang 6 Li nucleosynthesis studied deep underground (LUNA collaboration)

Trezzi

Anders

Aliotta

et al. 2017

Astroparticle Physics

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a b s t r a c tThe correct prediction of the abundances of the light nuclides produced during the epoch of Big Bang Nucleosynthesis (BBN) is one of the main topics of modern cosmology. For many of the nuclear reactions that are relevant for this epoch, direct experimental cross section data are available, ushering the so-called "age of precision". The present work addresses an exception to this current status: the 2 H( α, γ ) 6 Li reaction that controls 6 Li production in the Big Bang. Recent controversial observations of 6 Li in metal-poor stars have heightened the interest in understanding primordial 6 Li production. If confirmed, these observations would lead to a second cosmological lithium problem, in addition to the well-known 7 Li problem. In the present work, the direct experimental cross section data on 2 H( α, γ ) 6 Li in the BBN energy range are reported. The measurement has been performed deep underground at the LUNA (Laboratory for Underground Nuclear Astrophysics) 400 kV accelerator in the Laboratori Nazionali del Gran Sasso, Italy. The cross section has been directly measured at the energies of interest for Big Bang Nucleosynthesis for the first time, at E cm = 80, 93, 120, and 133 keV. Based on the new data, the 2 H( α, γ ) 6 Li thermonuclear reaction rate has been derived. Our rate is even lower than previously reported, thus increasing the discrepancy between predicted Big Bang 6 Li abundance and the amount of primordial 6 Li inferred from observations.

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Section: Thermonuclear Reaction Rate and Astrophysical Implicationscontrasting

confidence: 74%

Big Bang 6 Li nucleosynthesis studied deep underground (LUNA collaboration)

Trezzi

Anders

Aliotta

et al. 2017

Astroparticle Physics

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“…Metcalfe (2003) determined what the rates of the 12 C(α, γ) 16 O nuclear reaction needed to be in order to produce the carbon and oxygen abundance profiles infered from the asteroseismic study of GD 358 and CBS 114. For both stars, the rates found were consistent with the NACRE nuclear reaction rates (Angulo et al 1999). …”

Section: The 12 C(α γ) 16 O Ratesupporting

confidence: 83%

Constraints on stellar evolution from white dwarf asteroseismology

Kim

2014

Proc. IAU

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Abstract. High mass and low mass stars follow a similar evolution until the inert core phase that follows the end of the core helium burning stage. In particular, one common phase of stellar evolution is the alpha capture reaction that turns carbon into oxygen in the core. We can obtain constraints on this reaction rate by studying the remnants of low mass stars, as this is the ultimate reaction that occurs in their core. We also present results that allow us to test the time dependent calculations of diffusion in dense interiors.

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“…Actually, additional resonances might be populated in 20 Ne [32]. A recent experiment [33] measured the 19 F(p,α 0 ) 16 O astrophysical S (E)-factor by indirect means of the Trojan Horse method, and found that the largest rate difference, about 70%, occurs at temperatures relevant for post-AGB stars (∼0.1 GK), exceeding the upper limit set by the previous uncertainties [28]. Such difference is clearly due to the presence of the 113 keV resonance (E x =12.957 MeV, 2 + ).…”

Section: (Pα 0 ) Channelmentioning

confidence: 92%

“…However, these results were not included in the NACRE compilation as possible systematic errors affecting the absolute normalization might lead * Refer to five proposals submitted to NSFC in 2014, W.P. Liu et al, The 12 C(α,γ) 16 to an underestimate of S (E) by a factor of two [28]. The astrophysical factor was then extrapolated to low energies assuming a dominant contribution of the non-resonant part [28].…”

Section: (Pα 0 ) Channelmentioning

confidence: 99%

A proposed direct measurement of cross section at Gamow window for key reaction 19F(p,α) 16O in Asymptotic Giant Branch stars with a planned accelerator in CJPL

et al. 2016

Sci. China Phys. Mech. Astron.

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In 2014, the National Natural Science Foundation of China (NSFC) approved the Jinping Underground Nuclear Astrophysics laboratory (JUNA) project, which aims at direct cross-section measurements of four key stellar nuclear reactions right down to the Gamow windows. In order to solve the observed fluorine overabundances in Asymptotic Giant Branch (AGB) stars, measuring the key 19 F(p,α) 16 O reaction at effective burning energies (i.e., at Gamow window) is established as one of the scientific research sub-projects. The present paper describes this sub-project in details, including motivation, status, experimental setup, yield and background estimation, aboveground test, as well as other relevant reactions.Jinping Underground Nuclear Astrophysics laboratory (JUNA), direct measurement, Gamow window, cross section, AGB star, nucleosynthesis PACS number(s): 26.20.+f; 26.30.+k; 25.40.Ny, 27.20+n Citation:He J J, et al. A proposed direct measurement of cross section at Gamow window for key reaction 19 F(p,α) 16 O in Asymptotic Giant Branch stars with a planned accelerator in CJPL, Sci China-Phys Mech Astron, 2015, 58: 1-7, doi:

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A compilation of charged-particle induced thermonuclear reaction rates

Cited by 2,094 publications

References 525 publications

Big Bang 6 Li nucleosynthesis studied deep underground (LUNA collaboration)

Big Bang 6 Li nucleosynthesis studied deep underground (LUNA collaboration)

Constraints on stellar evolution from white dwarf asteroseismology

A proposed direct measurement of cross section at Gamow window for key reaction 19F(p,α) 16O in Asymptotic Giant Branch stars with a planned accelerator in CJPL

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