Scorpion, the Stuttgart scattering facility for fast polarized neutrons

Hammer, J. W.; Bulski, G.; Grum, W.; Krätschmer, Wolfgang; Postner, Harald; Schleussner, G.

doi:10.1016/0168-9002(86)91069-7

Cited by 10 publications

(1 citation statement)

References 26 publications

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“…JUNA Liu et al 2016) compared to LUNA 400. Efforts are underway to adopt and advance techniques from surface experiments, such as cooling for high-powered targets (Wolfgang Hammer et al, 1986) or largearea reaction targets (Chen et al, 2020), to overcome thermal limitations on the beam intensity in future underground experiments. Even with best efforts in cooling, the performance of solid targets degrades under the beam, which is seen, for example, in a reduction of target thickness or changes in the target stoichiometry.…”

Section: The MV Facility At Gran Sassomentioning

confidence: 99%

The Study of Key Reactions Shaping the Post-Main Sequence Evolution of Massive Stars in Underground Facilities

Ferraro

Ciani

Boeltzig

et al. 2021

Front. Astron. Space Sci.

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The chemical evolution of the Universe and several phases of stellar life are regulated by minute nuclear reactions. The key point for each of these reactions is the value of cross-sections at the energies at which they take place in stellar environments. Direct cross-section measurements are mainly hampered by the very low counting rate and by cosmic background; nevertheless, they have become possible by combining the best experimental techniques with the cosmic silence of an underground laboratory. In the nineties, the LUNA (Laboratory for Underground Nuclear Astrophysics) collaboration opened the era of underground nuclear astrophysics, installing first a homemade 50 kV and, later on, a second 400 kV accelerator under the Gran Sasso mountain in Italy: in 25 years of experimental activity, important reactions responsible for hydrogen burning could have been studied down to the relevant energies thanks to the high current proton and helium beams provided by the machines. The interest in the next and warmer stages of star evolution (i.e., post-main sequence and helium and carbon burning) drove a new project based on an ion accelerator in the MV range called LUNA-MV, able to deliver proton, helium, and carbon beams. The present contribution is aimed to discuss the state of the art for some selected key processes of post-main sequence stellar phases: 12C(α,γ)16O and 12C+12C are fundamental for helium and carbon burning phases, and 13C(α,n)16O and 22Ne(α,n)25Mg are relevant to the synthesis of heavy elements in AGB stars. The perspectives opened by an underground MV facility will be highlighted.

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Section: The MV Facility At Gran Sassomentioning

confidence: 99%