<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>E</mml:mi><mml:mn>1</mml:mn></mml:mrow></mml:math>and<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mrow><mml:mi>E</mml:mi><mml:mn>2</mml:mn></mml:mrow></mml:math>cross sections of the<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi mathvariant="normal">C</mml:mi><mml:mprescripts /><mml:none /><mml:mrow><mml:mn>12</mml:mn></mml:mrow>

Makii, H.; Nagai, Y.; Shima, T.; Segawa, M.; Mishima, Kenji; Ueda, Hiroshi; Igashira, M.; Ohsaki, T.

doi:10.1103/physrevc.80.065802

Cited by 45 publications

(156 citation statements)

References 38 publications

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“…The cross section for the triple-α process is experimentally quite well determined [4]. Our knowledge of the 12 C(α, γ) 16 O reaction under typical helium burning conditions (T 9 ∼ 0.2 or E c.m. ∼ 300 keV), however, is still limited by its small cross section and by the crucial role played by two sub-threshold states in 16 O [5].…”

Section: Introductionmentioning

confidence: 99%

“…Contrary to the triple α reaction which is dominated by the contribution from a resonant state (the so-called Hoyle state) the 12 C(α, γ) 16 O reaction proceeds mainly through two radiative capture modes to the 16 O ground state. One is E1 capture with contributions from the 1 − state at E x =9.585 MeV (E r =2.418 MeV) and the sub-threshold 1 − state at E x =7.117 MeV (E r =-45 keV).…”

Section: Introductionmentioning

confidence: 99%

“…The magnitude of this cross section, however, is still a hotly debated issue, both experimentally and theoretically, and many recent publications can be found in the literature [8,9,10,11,12,13,14,15,16].…”

Section: Introductionmentioning

confidence: 99%

“…Most of the carbon and oxygen which we observe today is produced by helium burning in red giant stars. These two elements are not only crucial for all living organisms, but their relative abundances, which are determined by the competition between the triple-α and the 12 C(α, γ) 16 O reactions, is also an important parameter for the evolution of a massive star at the end of its lifetime during the carbon-, neon-, and oxygen-burning phases [1,2,3]. The cross section for the triple-α process is experimentally quite well determined [4].…”

Section: Introductionmentioning

confidence: 99%

“…The isotopes 16 O and 12 C are, after 1 H and 4 He, the third and fourth most abundant nuclei in the visible universe. Most of the carbon and oxygen which we observe today is produced by helium burning in red giant stars.…”

Section: Introductionmentioning

confidence: 99%

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The Origin of Oxygen in the Universe - A new approach to an Old Question

Rehm

2012

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Abstract. Carbon and oxygen are not only important elements for the existence of life on Earth, but they also play an important role in the evolution of stars towards the end of their life cycle. The formation of 12 C through the so-called triple-α reaction is quite well understood. The next step, the formation of 16 O through the α capture reaction 12 C(α, γ) 16 O on the other hand, still has an experimental uncertainty of ∼ 30%. Direct measurements of the 12 C(α, γ) 16 O reaction by detecting either the outgoing γ radiation in a high acceptance Ge-detector array or the residual 16 O nuclei in a mass spectrometer do not allow for orderof-magnitude improvements. In this contribution, the possibility of using superheated bubble detectors for a measurement of the time-inverse 16 O(γ, α) 12 C reaction is being discussed. The first results of a 'proof-of-principle' experiment of the 19 F(γ, α) 15 N reaction are also being presented.

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Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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The Origin of Oxygen in the Universe - A new approach to an Old Question

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Fabrication of isotopic and natural carbon foils by thermal cracking method and some issues

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et al. 2015

J Radioanal Nucl Chem

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Recent progress in nuclear astrophysics research and its astrophysical implications at the China Institute of Atomic Energy

Liu,

Guo,

et al. 2024

NUCL SCI TECH

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Nuclear astrophysics is a rapidly developing interdisciplinary field of research that has received extensive attention from the scientific community since the mid-twentieth century. Broadly, it uses the laws of extremely small atomic nuclei to explain the evolution of the universe. Owing to the complexity of nucleosynthesis processes and our limited understanding of nuclear physics in astrophysical environments, several critical astrophysical problems remain unsolved. To achieve a better understanding of astrophysics, it is necessary to measure the cross sections of key nuclear reactions with the precision required by astrophysical models. Direct measurement of nuclear reaction cross sections is an important method of investigating how nuclear reactions influence stellar evolution. Given the challenges involved in measuring the extremely low cross sections of nuclear reactions in the Gamow peak and preparing radioactive targets, indirect methods, such as the transfer reaction, coulomb dissociation, and surrogate ratio methods, have been developed over the past several decades. These are powerful tools in the investigation of, for example, neutron-capture (n,$$\gamma$$ γ ) reactions with short-lived radioactive isotopes. However, direct measurement is still preferable, such as in the case of reactions involving light and stable nuclei. As an essential part of stellar evolution, these low-energy stable nuclear reactions have been of particular interest in recent years. To overcome the difficulties in measurements near or deeply within the Gamow window, the combination of an underground laboratory and high-exposure accelerator/detector complex is currently the optimal solution. Therefore, underground experiments have emerged as a new and promising direction of research. In addition, to better simulate the stellar environment in the laboratory, research on nuclear physics under laser-driven plasma conditions has gradually become a frontier hotspot. In recent years, the CIAE team conducted a series of distinctive nuclear astrophysics studies, relying on the Jinping Underground Nuclear Astrophysics platform and accelerators in Earth’s surface laboratories, including the Beijing Radioactive Ion beam Facility, as well as other scientific platforms at home and abroad. This research covered nuclear theories, numerical models, direct measurements, indirect measurements, and other novel approaches, achieving great interdisciplinary research results, with high-level academic publications and significant international impacts. This article reviews the above research and predicts future developments.

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E1andE2cross sections of theC12

Cited by 45 publications

References 38 publications

The Origin of Oxygen in the Universe - A new approach to an Old Question

The Origin of Oxygen in the Universe - A new approach to an Old Question

Fabrication of isotopic and natural carbon foils by thermal cracking method and some issues

Recent progress in nuclear astrophysics research and its astrophysical implications at the China Institute of Atomic Energy

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