Direct Mass Measurements of Short-Lived<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mi>A</mml:mi><mml:mo>=</mml:mo><mml:mn>2</mml:mn><mml:mi>Z</mml:mi><mml:mo>−</mml:mo><mml:mn>1</mml:mn></mml:math>Nuclides<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mmultiscripts><mml:mi>Ge</mml:mi><mml:mprescripts /><mml:none /><mml:mn>63</mml:mn></mml:mmultiscripts></mml:math>,<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mm

Tu, X. L.; Xu, Hu; Wang, M.; Zhang, Y.H.; Litvinov, Yu. A.; Sun, Y.; Schatz, H.; Zhou, Xianming; Yuan, Y.J.; Xia, J.W.; Audi, G.; Blaum, Klaus; Du, C. M.; Geng, Peng; Hu, Zhengguo; Huang, Weiling; Jin, S.; Liu, L.X.; Liu, Y.; Ma, Xueli; Mao, R.S.; Mei, B.; Peng, Shuai; Sun, Z. Y.; Suzuki, Hiroshi; Tang, S.W.; Wang, J.S.; Wang, S.T.; Xiao, Guoqing; Xu, X.; Yamaguchi, Takayuki; Yamaguchi, Yoshitaka; Yan, Xiao-Bo; Jiang, Yang; Ye, R.P.; Zang, Yunxiang; Zhao, Hongwei; Zhao, T.C.; Zhang, X.Y.; Wenlong, Zhan

doi:10.1103/physrevlett.106.112501

Cited by 173 publications

(52 citation statements)

References 30 publications

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“…Such range indicates that with the lower limit setting, a strong 64 Ge waiting point with maximum ratio of 1.1 cannot be ruled out as the flow of material almost accumulated at A = 64, and vice versa. Nevertheless, the minimum ratio of 0.2 signifies that 64 Ge is a weak waiting point, which is consistent with Tu et al [24].…”

Section: Astrophysical Implicationsupporting

confidence: 79%

“…In this contribution, we used the recently measured S p ( 65 As)= −90 ± 85 keV [23,24] and newly extrapolated S p ( 66 Se)= 1720±310 keV from Atomic Mass Evaluation 2012 (AME2012) [25] together with nuclear structure information estimated from large-scale shell-model calculations to deduce a new set of thermonuclear reaction rates of 64 Ge(p,γ) 65 As and 65 As(p,γ) 66 Se with identified uncertainties [26]. We compared our reaction rates with rates available in the JINA REACLIB database [27], i.e.…”

Section: Introductionmentioning

confidence: 99%

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New Reaction Rates Of 64Ge(p,γ)65As(p,γ)66Se And The Impact On Type I X-ray Bursts

Lam

Schatz

et al. 2017

Proceedings of the 26th International Nuclear Physics Conference — PoS(INPC2016)

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The nucleosynthesis occurring in type-I X-ray bursts (XRBs) and the respective energy released in these thermonuclear explosions are sensitive to nuclear masses and reaction rates around the 64 Ge waiting point. Based on the recently measured masses of 64 Ge and 65 As, the deduced proton separation energies S p ( 65 As) and S p ( 66 Se), and nuclear structure information from large-scale shell model calculations, we have obtained new reaction rates of 64 Ge(p, γ) 65 As and 65 As(p, γ) 66 Se with reliable uncertainties. Our new thermonuclear reaction rate of 64 Ge(p, γ) 65 As differs from those available in REACLIB by up to two orders of magnitude at temperature range associated with type-I X-ray bursts. We evaluated the impact of these new rates, particularly the energy generation and the burst light curve, with self-consistent one-zone model [Schatz et al. Phys. Rev. Lett. 86 (2001) 3471]. Also, we identified the nuclear physics uncertainties determining the role of the 64 Ge to be a waiting point in XRBs, and strongly affecting XRB model predictions of the synthesis of 64 Zn and the synthesis of nuclei A ≥ 64.

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Section: Astrophysical Implicationsupporting

confidence: 79%

Section: Introductionmentioning

confidence: 99%

New Reaction Rates Of 64Ge(p,γ)65As(p,γ)66Se And The Impact On Type I X-ray Bursts

Lam

Schatz

et al. 2017

Proceedings of the 26th International Nuclear Physics Conference — PoS(INPC2016)

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“…2, clearly demonstrate the importance of precise mass measurements for 76 Ni to 78 Ni. Using this approach, one can identify the key nuclei, including 76 Ni to 78 Ni, 82 Zn, 131 Cd, and 132 Cd [14]. These nuclei at neutron shells N=50 and 82 have the largest impact and are important candidates with high priority for precise mass measurements at rare-isotope beam (RIB) facilities.…”

Section: Nuclear Mass and Precisionmentioning

confidence: 99%

“…112 Sn beams. A typical precision of less than 50 keV was obtained by confining the data analysis to the "isochronous" part [82,83]. Masses of 16 neutrondeficient nuclides were obtained for the first time [84].…”

Section: The Achievable Relative Precision Of Pmts With the Tof-icr Tmentioning

confidence: 99%

Toward precision mass measurements of neutron-rich nuclei relevant to r-process nucleosynthesis

et al. 2015

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The open question of where, when, and how the heavy elements beyond iron enrich our Universe has triggered a new era in nuclear physics studies. Of all the relevant nuclear physics inputs, the mass of very neutron-rich nuclides is a key quantity for revealing the origin of heavy elements beyond iron. Although the precise determination of this property is a great challenge, enormous progress has been made in recent decades, and it has contributed significantly to both nuclear structure and astrophysical nucleosynthesis studies. In this review, we first survey our present knowledge of the nuclear mass surface, emphasizing the importance of nuclear mass precision in r-process calculations. We then discuss recent progress in various methods of nuclear mass measurement with a few selected examples. For each method, we focus on recent breakthroughs and discuss possible ways of improving the weighing of r-process nuclides.

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“…China now has two world-class facilities of this kind, the Lanzhou Cooler Storage Ring (CSR) and the Beijing HI-13 Tandem accelerator which will be upgraded to Rare Ion-Beam Facility in Beijing (BRIF) in 2014. While the Lanzhou CSR has begun to produce exciting results in the mass measurement [8][9][10][11], the Beijing HI-13 Tandem Laboratory has also performed an important experiment for determination of the 13 C(,n) 16 O reaction rate [12].…”

mentioning

confidence: 99%

A new era of nuclear astrophysics research in China

Sun

Liu

2012

Chin. Sci. Bull.

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Nuclear astrophysics is a rapidly-growing interdisciplinary branch of physics involving a close collaboration among researchers in nuclear physics, astrophysics, and observational astronomy. The origin and fate of matter in our Universe are the primary questions in the nuclear astrophysics research [1,2], which, to large extent, have not been understood. In particular, the question of how heavy elements in the Universe (those heavier than iron) were created is one of the major unsolved puzzles in physics [3]. The above-mentioned fields are connected together because many important signatures of the microscopic nuclear processes of element production can directly be observed in cosmic phenomena. For example, the light curves of supernova and X-ray burst explosions contain information on the energy release from nuclear reactions [4]. Freshly-synthesized elements through various nuclear processes in stars can be detected through atomic absorption and emission lines, or, in some radioactive species, through characteristic gamma radiation. Thus, our desire of understanding the cosmos on the femto-scale while interpreting astrophysical observations on the tera-scale [5] creates a momentum which has propelled the field of nuclear astrophysics to the research forefront. Moreover, since most of the astrophysical processes of nucleosynthesis take place along the lines of extremely unstable nuclei in the nuclear chart, our knowledge on the basic nuclear properties has to be extended to those exotic nuclei, which is by itself a frontier of nuclear physics.For the following reasons, now it seems to be a golden time for this research that crosses over several disciplines. The large collection of observational data from both ground-and space-based telescopes offers a wealth of information which needs to be interpreted by detailed theoretical modeling of complex hydrodynamic and nuclear processes. Rapidly-expanding computational capabilities and novel numerical techniques allow more realistic treatments of evolutionary processes in stars. Advances in experimental nuclear physics enable us to probe and simulate the behavior of nuclei under extreme conditions to understand the nuclear processes behind the cosmic phenomena. These exotic nuclear processes that play crucial roles in astronomical observations are defined in a wide range, including, for example, low energy charged particle reactions in the stellar interiors, thermo-nuclear reactions of extremely short-lived nuclei in stellar explosions, neutrino-nucleus interactions in the early supernova shock, and nuclear fusion processes induced by the extreme densities in neutron stars.

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Direct Mass Measurements of Short-LivedA=2Z−1NuclidesGe63,

Cited by 173 publications

References 30 publications

New Reaction Rates Of 64Ge(p,γ)65As(p,γ)66Se And The Impact On Type I X-ray Bursts

New Reaction Rates Of 64Ge(p,γ)65As(p,γ)66Se And The Impact On Type I X-ray Bursts

Toward precision mass measurements of neutron-rich nuclei relevant to r-process nucleosynthesis

A new era of nuclear astrophysics research in China

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