Measurements of the Coulomb dissociation cross section of 156 MeV<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mmultiscripts><mml:mrow><mml:mi mathvariant="normal">Li</mml:mi></mml:mrow><mml:mprescripts /><mml:mrow /><mml:mrow><mml:mn>6</mml:mn></mml:mrow><mml:mrow /><mml:mrow /></mml:mmultiscripts></mml:mrow></mml:math>projectiles at extremely low relative fragment energies of astrophysical interest

Kiener, J.; Gils, H.J.; Rebel, H.; Zagromski, S.; Gsottschneider, G.; Heide, N.; Jelitto, Hans; Wentz, J.; Baur, G.

doi:10.1103/physrevc.44.2195

Cited by 137 publications

(230 citation statements)

References 33 publications

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“…The LUNA data (method B analysis, see Table 2 ) are reported in red. The cross section measured at E cm = 80 keV and E cm = 93 keV are shown as upper limits (90% confidence level) because the experimental results are compatible with zero within two σ s. The previous measurements and upper limits are also reported: blue triangles [19] , green circle [18] , black arrows [20] (upper limits), blue dashed arrow [17] (upper limits). Also shown is our recommended total cross section curve (red full line), together with the adopted E2 component [15] and the E1 component derived from LUNA data (see text).…”

Section: Thermonuclear Reaction Rate and Astrophysical Implicationsmentioning

confidence: 77%

“…However, the competing nuclear breakup process dominates at both beam energies [15,20] . Therefore, these data may be interpreted as upper limits of the E2 contribution to the cross section.…”

Section: The Nuclear Physics Of Primordial 6 LImentioning

confidence: 99%

“…around the 711 keV resonance [18] , and in the MeV region [19] . In order to unfold the 2 H( α, γ ) 6 Li cross section at low energy, two different Coulomb dissociation experiments have been performed at 26 [20] and 150 MeV/nucleon [15] projectile energy, respectively. (4) is below the calorimeter.…”

Section: The Nuclear Physics Of Primordial 6 LImentioning

confidence: 99%

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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 Implicationsmentioning

confidence: 77%

Section: The Nuclear Physics Of Primordial 6 LImentioning

confidence: 99%

See 1 more Smart Citation

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

Trezzi

Anders

Aliotta

et al. 2017

Astroparticle Physics

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show abstract

“…Note that formally we can obtain the overlap function with the same ANC as in [2] by multiplying the boundstate wave function generated by the potential V (r) on the square root of the proper spectroscopic factor. However, this procedure is not legitimate, as it has been discussed above, because potential V (r) fits the elastic scattering [20]; black crosses are data from [24]; black triangles are data from [27]. The red solid line is the S24(E) factor from [21].…”

Section: Inverse Scattering Problem Bound-state Potential and Ancmentioning

confidence: 99%

“…The first indirect information about the astrophysical factor S 24 (E) for the α+d → 6 Li+γ process has been obtained in [20] from the Coulomb breakup process 208 Pb( 6 Li (26A MeV), α d) 208 Pb. The analysis of the data was performed under assumption that the reaction mechanism is contributed purely by the Coulomb breakup.…”

Section: Introductionmentioning

confidence: 99%