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Leva, A. Di; Gialanella, L.; Kunz, Ralf; Rogalla, D.; Schürmann, D.; Strieder, F.; Cesare, M. De; Cesare, N. De; D’Onofrio, Antonio; Fülöp, Zs.; Gyürky, Gy.; Imbriani, G.; Mangano, Gianpiero; Ordine, A.; Roca, V.; Rolfs, C.; Somorjai, E.; Terrasi, F.

doi:10.1103/physrevlett.103.159903

Cited by 74 publications

(216 citation statements)

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“…∼700-2800 keV by using the activation method. Three data points obtained with low statistical error contribution [15] particularly show a good agreement with the ERNA data [11] and disagree with those from Parker et al [10]. A good agreement of our results and those from the ERNA collaboration is also seen when comparing with the recent measurements obtained by the ATOMKI collaboration using the activation technique [16].…”

Section: Introductionsupporting

confidence: 76%

“…The brown filled circle shows the value obtained using the activation technique at TRIUMF. The S factors from Parker et al [10] and LUNA [22,23], ERNA [11], ATOMKI [16], Weizmann [21], Notre Dame [24] and Seattle [25] collaborations are also shown for comparison.…”

Section: Analysis and Resultsmentioning

confidence: 99%

“…Large discrepancies are observed in the region 1000-3000 keV, where only data from Parker et al [10] and the ERNA collaboration [11] were available before the measurements performed by our collaboration. Also, discrepancies are seen in the same energy region when comparing different calculations, e.g.…”

Section: Introductionmentioning

confidence: 98%

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Constraining the Astrophysical S Factor of the ³He(α,γ)⁷Be Reaction

Carmona-Gallardo

Rojas

Singh

et al. 2015

Proceedings of the Conference on Advances in Radioactive Isotope Science (ARIS2014)

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The cross section of the 3 He(α,γ) 7 Be reaction has been widely studied both from the theoretical and the experimental fronts due to its relevance to the standard solar model and to the Big Bang Nucleosynthesis calculations. We report here on cross section measurements in the energy region E c.m. =1-3 MeV using the direct recoil counting method in an attempt to resolve the discrepancies among the previous data sets and calculations in this energy region and thus to constrain the extrapolations of the S 34 (E) curve to astrophysical energies.

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Section: Introductionsupporting

confidence: 76%

Section: Analysis and Resultsmentioning

confidence: 99%

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Constraining the Astrophysical S Factor of the ³He(α,γ)⁷Be Reaction

Carmona-Gallardo

Rojas

Singh

et al. 2015

Proceedings of the Conference on Advances in Radioactive Isotope Science (ARIS2014)

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“…A revision of this reaction rate therefore looks mandatory for minimizing the uncertainty on the 19 F nucleosynthesis related to this nuclear process. We will clarify this issue in the near future, when we directly measure the strength of the 364 keV resonance and the intensity of the DC component using the ERNA recoil separator (Schürmann et al 2005;di Leva et al 2009;Di Leva et al 2012). …”

Section: Exploration Above Current Experimental Uncertaintiesmentioning

confidence: 99%

Effects of nuclear cross sections on¹⁹F nucleosynthesis at low metallicities

Cristallo

Leva

Imbriani

et al. 2014

A&A

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Context. The origin of fluorine is a longstanding problem in nuclear astrophysics. It is widely recognized that asymptotic giant branch (AGB) stars are among the most important contributors to the Galactic fluorine production. Aims. In general, extant nucleosynthesis models overestimate the fluorine production by AGB stars with respect to observations. Although those differences are rather small at solar metallicity, low metallicity AGB stellar models predict fluorine surface abundances up to one order of magnitude larger than the observed ones. Methods. As part of a project devoted to reducing the uncertainties in the nuclear physics that affect the nucleosynthesis in AGB stellar models, we review the relevant nuclear reaction rates involved in the fluorine production or destruction. We perform this analysis on a model with initial mass M = 2 M and Z = 0.001. Results. We found that the major uncertainties are due to the 13 C(α,n) 16 O, the 19 F(α,p) 22 Ne, and the 14 N(p,γ) 15 O reactions. A change in the corresponding reaction rates within the present experimental uncertainties implies surface 19 F variations at the AGB tip lower than 10%, thus much smaller than observational uncertainties. For some α capture reactions, however, cross sections at astrophysically relevant energies are determined on the basis of nuclear models, in which some low-energy resonance parameters are very poorly known. Thus, larger variations in the rates of those processes cannot be excluded. That being so, we explore the effects of the variation in some α capture rates well beyond the current published uncertainties. The largest 19 F variations are obtained by varying the 15 N(α,γ) 19 F and the 19 F(α,p) 22 Ne reactions. Conclusions. The currently estimated uncertainties of the nuclear reaction rates involved in the production and destruction of fluorine produce minor 19 F variations in the ejecta of AGB stars. Analysis of some α capture processes that assume a wider uncertainty range determines 19 F abundances in better agreement with recent spectroscopic fluorine measurements at low metallicity. In the framework of this scenario, the 15 N(α,γ) 19 F and the 19 F(α,p) 22 Ne reactions show the strongest effects on fluorine nucleosynthesis. The presence of poorly known low-energy resonances make such a scenario possible, even if it is unlikely. We plan to measure these resonances directly.

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“…Our precise results clearly rule out the 3 He( 4 He,) 7 Be cross section as a possible source of the discrepancy between the predicted primordial 7 Li abundance and its much lower observed value. The LUNA results and few other high precision measurements [27,28,29] were included in the recent compilation "Solar fusion II" [30] to derive the best astrophysical S-factor for the 3 He( 4 He,) 7 Be reaction. The value obtained allows for a uncertainty reduction in the solar neutrino fluxes from 7.5% to 4.3% in the case of 8 B and from 8% to 4.5% in the case of 7 Be [31].…”

Section: Be Reactionmentioning

confidence: 99%

Recent results on (p,γ) and (α,γ) fusion reactions at LUNA

Guglielmetti

2011

EPJ Web of Conferences

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Abstract. At temperatures typical of astrophysical environments, nuclear cross sections are extremely small and experimental measurements in a laboratory at the Earth's surface are hampered by the cosmic background. The LUNA collaboration has exploited the unique features of background reduction offered by the rock overburden above the LNGS underground laboratory in order to study very important hydrogen-burning reactions at their relevant astrophysical energies. After a general introduction on the LUNA experiment, this paper reports on the most important results for the (p,) and (,) fusion reactions measured so far and their astrophysical consequences. A quick look on the future possibilities is also given.

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Erratum: Stellar and Primordial Nucleosynthesis ofBe7: Measurement ofHe3(α,<

Cited by 74 publications

References 0 publications

Constraining the Astrophysical S Factor of the ³He(α,γ)⁷Be Reaction

Constraining the Astrophysical S Factor of the ³He(α,γ)⁷Be Reaction

Effects of nuclear cross sections on¹⁹F nucleosynthesis at low metallicities

Recent results on (p,γ) and (α,γ) fusion reactions at LUNA

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Erratum: Stellar and Primordial Nucleosynthesis ofBe7: Measurement ofHe3(α,<

Cited by 74 publications

References 0 publications

Constraining the Astrophysical S Factor of the 3He(α,γ)7Be Reaction

Constraining the Astrophysical S Factor of the 3He(α,γ)7Be Reaction

Effects of nuclear cross sections on19F nucleosynthesis at low metallicities

Recent results on (p,γ) and (α,γ) fusion reactions at LUNA

Contact Info

Product

Resources

About

Constraining the Astrophysical S Factor of the ³He(α,γ)⁷Be Reaction

Constraining the Astrophysical S Factor of the ³He(α,γ)⁷Be Reaction

Effects of nuclear cross sections on¹⁹F nucleosynthesis at low metallicities