Rohrleitungen

Schröder, Karl

doi:10.1007/978-3-642-52099-0_7

Cited by 8 publications

(18 citation statements)

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“…2). Contrary to [9] for capture to the ground state, they reported a negligible contribution due to a smaller total width of the subthreshold resonance. Subsequently, the data of Schroder et al [9] were reanalyzed by [10] using an R-matrix approach.…”

Section: The 14 N(p Y) Ls O Reaction Measurementmentioning

confidence: 78%

“…The capture cross section needs to be known down to Eo=30 keV (the Gamow peak in core H-burning stars), which is far below the low-energy limit of direct y-ray measurements, i.e. According to the data and analysis of [9], there are two major and nearly equal contributions to S(0): the direct capture (DC) to the 6.79 MeV state in 15 0 and the capture to the ground state (gs) in 15 0 ( fig. Thus, the data had to be extrapolated over a large energy gap leading to a substantial uncertainty for the astrophysical S-factor at zero energy, S(0).…”

Section: The 14 N(p Y) Ls O Reaction Measurementmentioning

confidence: 99%

“…Thus, the data had to be extrapolated over a large energy gap leading to a substantial uncertainty for the astrophysical S-factor at zero energy, S(0). The latter process is enhanced due to a subthreshold resonance at E R =-507 keV, the width of which was taken as a free parameter in the fit [9]. 2).…”

Section: The 14 N(p Y) Ls O Reaction Measurementmentioning

confidence: 99%

“…According to the data and analysis of [9], there are two major and nearly equal contributions to S(0): the direct capture (DC) to the 6.79 MeV state in 15 0 and the capture to the ground state (gs) in 15 0 ( fig. Subsequently, the data of Schroder et al [9] were reanalyzed by [10] using an R-matrix approach. The latter process is enhanced due to a subthreshold resonance at E R =-507 keV, the width of which was taken as a free parameter in the fit [9].…”

Section: The 14 N(p Y) Ls O Reaction Measurementmentioning

confidence: 99%

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Underground studies of pp and CNO

Costantini¹

2007

AIP Conference Proceedings

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Section: The 14 N(p Y) Ls O Reaction Measurementmentioning

confidence: 78%

Section: The 14 N(p Y) Ls O Reaction Measurementmentioning

confidence: 99%

Section: The 14 N(p Y) Ls O Reaction Measurementmentioning

confidence: 99%

Section: The 14 N(p Y) Ls O Reaction Measurementmentioning

confidence: 99%

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Underground studies of pp and CNO

Costantini¹

2007

AIP Conference Proceedings

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“…However, data points at higher energy are also necessary to obtain a reliable R-matrix fit and extrapolation of the S-factor S(0). Therefore, and in order to obtain an independent verification of the high energy Schröder et al data [8], the reaction is re-studied here. The cross section for capture to different excited states and to the ground state of 15 O has been studied and S-factor data have been provided, together with theoretical fits, recommending S tot (0) = 3.2 keV·barn.…”

Section: Introductionmentioning

confidence: 99%

The [sup 14]N(p,γ)[sup 15]O reaction studied at high energy

Marta

Spitaleri²,

Rolfs³

et al. 2010

AIP Conference Proceedings

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The 14 N(p,γ) 15 O reaction is the bottleneck of the carbon-nitrogen-oxygen (CNO) cycle. Recent studies of this reaction have been performed in the low energy range E < 500 keV. However, also data at higher energy are necessary to extrapolate the S-factor down to the energy range of astrophysical interest. Up to now, only one set of data from an experiment performed in 1987 extends up to 2.5 MeV. A new study has been carried out at the high-current FZD Tandetron in Dresden, in the energy region from 0.6 to 2.5 MeV. The astrophysics motivations, setup and on-going analysis are presented.

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LUNA: Status and prospects

Broggini

Bemmerer

Caciolli

et al. 2018

Progress in Particle and Nuclear Physics

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The essential ingredients of nuclear astrophysics are the thermonuclear reactions which shape the life and death of stars and which are responsible for the synthesis of the chemical elements in the Universe. Deep underground in the Gran Sasso Laboratory the cross sections of the key reactions responsible for the hydrogen burning in stars have been measured with two accelerators of 50 and 400 kV voltage right down to the energies of astrophysical interest. As a matter of fact, the main advantage of the underground laboratory is the reduction of the background. Such a reduction has allowed, for the first time, to measure relevant cross sections at the Gamow energy. The qualifying features of underground nuclear astrophysics are exhaustively reviewed before discussing the current LUNA program which is mainly devoted to the study of the Big-Bang nucleosynthesis and of the synthesis of the light elements in AGB stars and classical novae. The main results obtained during the study of reactions relevant to the Sun are also reviewed and their influence on our understanding of the properties of the neutrino, of the Sun and of the Universe itself is discussed. Finally, the future of LUNA during the next decade is outlined. It will be mainly focused on the study of the nuclear burning stages after hydrogen burning: helium and carbon burning. All this will be accomplished thanks to a new 3.5 MV accelerator able to deliver high current beams of proton, helium and carbon which will start running under Gran Sasso in 2019. In particular, we will discuss the first phase of the scientific case of the 3.5 MV accelerator focused on the study of 12 C+ 12 C and of the two reactions which generate free neutrons inside stars: 13 C(α,n) 16 O and 22 Ne(α,n) 25 Mg. arXiv:1707.07952v4 [nucl-ex]

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Rohrleitungen

Cited by 8 publications

References 0 publications

Underground studies of pp and CNO

Underground studies of pp and CNO

The [sup 14]N(p,γ)[sup 15]O reaction studied at high energy

LUNA: Status and prospects

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