Cross section of the reaction 6Li(p, γ)7Be

Switkowski, Z.E.; Heggie, J.C.P.; Kennedy, D.L.; Sargood, D.G.; Barker, F.C.; Spear, R.H.

doi:10.1016/0375-9474(79)90300-2

Cited by 53 publications

(99 citation statements)

References 7 publications

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“…A recent review [3] suggests the predicted 7 Li abundances are 2-4 times higher than those measured, and inversely the predicted 6 Li abundances are 5000 times lower than measured. Whilst this large discrepancy is currently attributed to 6 Li production via proton induced spallation and fusion reactions, the environments encountered in PMS stars are expected to destroy more 6 Li than 7 Li. To further constrain the predicted abundances of 6 Li in PMS stars, further high accuracy measurements are required of the reactions burning 6 Li.…”

Section: Introductionmentioning

confidence: 90%

“…Of high interest to nuclear astrophysicists, the parameters obtained from BBN+WMAP data have been used to predict the present abundances of low mass isotopes found in stars. Whilst deuterium and 4 He abundances show excellent agreement between those predicted by BBN+WMAP and those measured in galaxies [2], large discrepancies are found for 6 Li and 7 Li between BBN+WMAP predictions and measurements of low-metallicity, or pre-main sequence (PMS), stars. A recent review [3] suggests the predicted 7 Li abundances are 2-4 times higher than those measured, and inversely the predicted 6 Li abundances are 5000 times lower than measured.…”

Section: Introductionmentioning

confidence: 99%

“…Whilst deuterium and 4 He abundances show excellent agreement between those predicted by BBN+WMAP and those measured in galaxies [2], large discrepancies are found for 6 Li and 7 Li between BBN+WMAP predictions and measurements of low-metallicity, or pre-main sequence (PMS), stars. A recent review [3] suggests the predicted 7 Li abundances are 2-4 times higher than those measured, and inversely the predicted 6 Li abundances are 5000 times lower than measured. Whilst this large discrepancy is currently attributed to 6 Li production via proton induced spallation and fusion reactions, the environments encountered in PMS stars are expected to destroy more 6 Li than 7 Li.…”

Section: Introductionmentioning

confidence: 99%

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Proton-Induced Reactions of Astrophysical Interest

Chillery

2018

EPJ Web Conf.

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Abstract. A discrepancy exists between the 6 Li abundances predicted from big bang nucleosynthesis models and those measured in pre-main sequence stars. To further constrain the predicted abundances of 6 Li in these stars, high accuracy measurements are required of reactions destroying 6 Li. Namely 6 Li(p,γ) 7 Be and 6 Li(p,α) 3 He. These have recently been studied at the Laboratory for Underground Nuclear Astrophysics (LUNA) to measure their low energy cross sections. I present both the campaign's experimental setup and current status of the data analysis.

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Section: Introductionmentioning

confidence: 90%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Proton-Induced Reactions of Astrophysical Interest

Chillery

2018

EPJ Web Conf.

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“…to the final bound state J f = 3/2 experimental data [13][14][15] and other theoretical studies [16,17]. Switkowski et al [13] measured 6 Li(p, γ) 7 Be cross section over a wide energy range of astrophysical interest.…”

Section: All Relevant E1 M1 E2 Transitions From the Initial Continumentioning

confidence: 97%

“…Switkowski et al [13] measured 6 Li(p, γ) 7 Be cross section over a wide energy range of astrophysical interest. These data are well described by the GSM-CC calculations except for the lowest experimental point at E CM = 140 keV.…”

Section: All Relevant E1 M1 E2 Transitions From the Initial Continumentioning

confidence: 99%

AstrophysicalS-factor for⁶Li(ρ, γ)⁷Be in the coupled-channel Gamow shell model

Dong

Fossez

Michel

et al. 2016

EPJ Web of Conferences

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Abstract. We have applied the Gamow shell model (GSM) in the coupled-channel representation to study the astrophysical S -factor for the proton radiative capture reaction of 6 Li. Reaction channels are built by coupling the proton wave function expanded in different partial waves with the GSM wave functions of the ground state (1 + ) and the excited states (3 + 1 , 0 + 1 and 2 + 1 ) of 6 Li. All relevant E1, M1, and E2 transitions from the initial continuum states in 7 Be to the final bound states (3/2 − 1 and 1/2 − 1 ) are included. It is found that the calculated total astrophysical S factor for this reaction agrees well with the experimental data.

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