Program and status for the planned underground accelerator in the Dresden Felsenkeller

Bemmerer, D.; Akhmadaliev, Shavkat; Al-Abdullah, T.; Anders, M.; Cowan, T. E.; Elekes, Z.; Junghans, A. R.; Gohl, Stefan; Krause, Jörg; Reinhardt, Tobias P.; Reinicke, Stefan; Rimarzig, B.; Röder, M.; Schmidt, K.; Schwengner, R.; Szücs, T.; Takács, M. P.; Wagner, Andreas; Wagner, Louis K.; Wielicki, J; Zuber, Κ.

doi:10.1088/1742-6596/665/1/012030

Cited by 3 publications

(4 citation statements)

References 19 publications

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“…For these cases, a new comprehensive data set connecting the precise lowenergy LUNA [24,25,27,28] with the wide energy range Bochum data points is still missing. Due to the long running times and low counting rates, such data can best be provided at one of the upcoming higher-energy underground accelerators [59][60][61][62].…”

Section: Discussionmentioning

confidence: 99%

Astrophysical S factor of the N14(p,γ)O15

et al. 2018

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The 14 N(p,γ) 15 O reaction is the slowest reaction of the carbon-nitrogen cycle of hydrogen burning and thus determines its rate. The precise knowledge of its rate is required to correctly model hydrogen burning in asymptotic giant branch stars. In addition, it is a necessary ingredient for a possible solution of the solar abundance problem by using the solar 13 N and 15 O neutrino fluxes as probes of the carbon and nitrogen abundances in the solar core. After the downward revision of its cross section due to a much lower contribution by one particular transition, capture to the ground state in 15 O, the evaluated total uncertainty is still 8%, in part due to an unsatisfactory knowledge of the excitation function over a wide energy range. The present work reports precise S-factor data at twelve energies between 0.357-1.292 MeV for the strongest transition, capture to the 6.79 MeV excited state in 15 O, and at ten energies between 0.479-1.202 MeV for the second strongest transition, capture to the ground state in 15 O. An R-matrix fit is performed to estimate the impact of the new data on astrophysical energies. The recently suggested slight enhancement of the 6.79 MeV transition at low energy could not be confirmed. The present extrapolated zero-energy S-factors are S6.79(0) = 1.24±0.11 keV barn and SGS(0) = 0.19±0.05 keV barn.

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Section: Discussionmentioning

confidence: 99%

Astrophysical S factor of the N14(p,γ)O15

et al. 2018

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“…The present contribution reports on the status of the Felsenkeller shallow-underground accelerator for nuclear astrophysics, updating Ref. [24].…”

Section: Scientific Motivationmentioning

confidence: 99%

The new Felsenkeller 5 MV underground accelerator

et al. 2019

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The field of nuclear astrophysics is devoted to the study of the creation of the chemical elements. By nature, it is deeply intertwined with the physics of the Sun. The nuclear reactions of the proton-proton cycle of hydrogen burning, including the 3 He(α,γ) 7 Be reaction, provide the necessary nuclear energy to prevent the gravitational collapse of the Sun and give rise to the by now wellstudied pp, 7 Be, and 8 B solar neutrinos. The not yet measured flux of 13 N, 15 O, and 17 F neutrinos from the carbon-nitrogen-oxygen cycle is affected in rate by the 14 N(p,γ) 15 O reaction and in emission profile by the 12 C(p,γ) 13 N reaction. The nucleosynthetic output of the subsequent phase in stellar evolution, helium burning, is controlled by the 12 C(α,γ) 16 O reaction.In order to properly interpret the existing and upcoming solar neutrino data, precise nuclear physics information is needed. For nuclear reactions between light, stable nuclei, the best available technique are experiments with small ion accelerators in underground, low-background settings. The pioneering work in this regard has been done by the LUNA collaboration at Gran Sasso/Italy, using a 0.4 MV accelerator.The present contribution reports on a higher-energy, 5.0 MV, underground accelerator in the Felsenkeller underground site in Dresden/Germany. Results from γ-ray, neutron, and muon background measurements in the Felsenkeller underground site in Dresden, Germany, show that the background conditions are satisfactory for nuclear astrophysics purposes. The accelerator is in the commissioning phase and will provide intense, up to 50 µA, beams of 1 H + , 4 He + , and 12 C + ions, enabling research on astrophysically relevant nuclear reactions with unprecedented sensitivity.

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“…The first application of muon flux measurements was at a proposed place of a future underground laboratory at Felsenkeller Dresden Germany. Here nuclear astrophysical processes will be investigated by an accelerator-based experiment [114]. The aim of the muon flux measurements was to determine the cosmic background of the proposed experiments and to find the best location for the detectors where the cosmic background is minimal.…”

Section: Cosmic Background Measurements Of Proposed Experimentsmentioning

confidence: 99%

“…The aim of the muon flux measurements was to determine the cosmic background of the proposed experiments and to find the best location for the detectors where the cosmic background is minimal. Figure 74 shows the schematic of the tunnels in Felsenkeller [114]. The detector was deployed at the end of Tunnel IX at the proposed place of the Pelletron.…”

Section: Cosmic Background Measurements Of Proposed Experimentsmentioning

confidence: 99%

Research and development of particle detectors for muon tomography and the CERN ALICE experiment

Oláh¹

2016

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Program and status for the planned underground accelerator in the Dresden Felsenkeller

Abstract: Abstract. The scientific program and curent status of the planned accelerator laboratory in the Felsenkeller shallow-underground facility in Dresden, Germany, are reviewed.

Cited by 3 publications

References 19 publications

Astrophysical S factor of the N14(p,γ)O15

Astrophysical S factor of the N14(p,γ)O15

The new Felsenkeller 5 MV underground accelerator

Research and development of particle detectors for muon tomography and the CERN ALICE experiment

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