Progress of Jinping Underground laboratory for Nuclear Astrophysics (JUNA)

Liu, Weiping; Li, Zhihong; He, J. J.; Tang, Xiaodong; Liu, Gang; An, Zhu; Chang, Jui-Jen; Chen, Han; Chen, Qinghao; Chen, Xiongjun; Chen, Zhijun; Cui, Baoqun; Du, Xianchao; Fu, Changbo; Lin, Ge; He, Guo‐Zhong; Heger, Alexander; Suqing, Hou; Huang, Hanxiong; Huang, Ning; Jia, Bei; Jiang, Liyang; Kubono, S.; Li, Jianmin; Kuoang, Li; Li, Tao; Li, Yunju; Lugaro, Maria; Ma, Hui; Ma, S.; Mei, Dongming; Qian, Yongzhong; Jiuchang, Qin; Ren, Jie; Shen, Y. P.; Su, J.; Sun, Limin; Tan, Wanpeng; Tanihata, Isao; Wang, Shuo; Wang, Peng; Wang, Youbao; Wu, Qi; Xu, Shutao; Yan, S. Q.; Yang, L.; Yang, Y.; Yu, Xiao; Yue, Qian; Zeng, Sheng; Zhang, Huanyu; Zhang, Hui; Zhang, LiYong; Zhang, Ningtao; Zhang, Qiwei; Zhang, Tao; Zhang, Xiao-Peng; Zhang, Xuezhen; Zhang, Ziming; Zhao, Wei; Zuo, Zhihong; Zhou, Chao

doi:10.1051/epjconf/201610909001

Cited by 10 publications

(34 citation statements)

References 21 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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“…Direct measurements in nuclear astrophysics benefit from an 6 underground environment, which greatly reduces cosmic ray induced background. The Jinping Underground laboratory for Nuclear Astrophysics (JUNA) [24] in China, which is being constructed and expected to deliver beam in a few years, would be a proper place to do the 12 C+ 12 C measurement with the ultra-low background of the China Jinping Underground Laboratory (CJPL) [25].…”

Section: Discussionmentioning

confidence: 99%

An efficient method for mapping the $${}^{12}\hbox {C}+{}^{12}\hbox {C}$$ molecular resonances at low energies

Tang

Fang

et al. 2019

NUCL SCI TECH

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The 12 C+ 12 C fusion reaction is famous for its complication of molecular resonances, and plays an important role in both nuclear structure and astrophysics. It is extremely difficult to measure the cross sections of 12 C+ 12 C fusions at energies of astrophysical relevance due to very low reaction yields. To measure the complicated resonant structure existing in this important reaction, an efficient thick target method has been developed and applied for the first time at energies Ec.m.<5.3 MeV. A scan of the cross sections over a relatively wide range of energies can be carried out using only a single beam energy. The result of measurement at Ec.m.= 4.1 MeV is compared with other results from previous work. This method would be useful for searching potentially existing resonances of 12 C+ 12 C in the energy range 1 MeV

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“…The limited energy range of the unique LUNA 0.4 MV underground accelerator has led to a call for new, higher-energy underground accelerators [19,20]. As a result, new underground accelerator laboratories are under construction or starting up on three continents: The LUNA-MV 3.5 MV accelerator in Gran Sasso, Italy [21], the CASPAR 1 MV accelerator in Lead, South Dakota, USA [22], and the JUNA accelerator complex in the Jinping laboratory, China [23].…”

Section: Scientific Motivationmentioning

confidence: 99%

“…The most recent example is the 22 Ne(p,γ) 23 Na reaction, where owing to the low background underground three new resonances have been discovered [15,16] and two hypothetical resonances ruled out experimentally [17]. These data address the well-known anticorrelation of sodium and oxygen abundances in globular cluster stars [18].…”

Section: Introductionmentioning

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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Progress of Jinping Underground laboratory for Nuclear Astrophysics (JUNA)

Cited by 10 publications

References 21 publications

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

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

An efficient method for mapping the $${}^{12}\hbox {C}+{}^{12}\hbox {C}$$ molecular resonances at low energies

The new Felsenkeller 5 MV underground accelerator

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