First mass measurement of short-lived nuclides at HIRFL-CSR

Xu, H. S.; Tu, X. L.; Yuan, Y.J.; Xia, J.W.; Yong-Dong, Zang; Wang, Meng; Mao, Ruishi; Hu, Zhiyun; Mei, B.; Peng, Shuai; Zhu, Zhichao; Tang, S.W.; Geng, Peng; Liu, Yong; Zhao, T.C.; Zhang, Xueying; Jiang, Yang; Mao, Lijun; Zhang, Yuhu; Zhou, X. H.; Huang, Wenxue; Xiao, Guoqing; Zhao, Hongwei; Wenlong, Zhan

doi:10.1007/s11434-009-0719-9

Cited by 23 publications

(14 citation statements)

References 15 publications

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“…Restricting the acceptance of the injected beam in the IMS experiments allows increasing of the resolving power [72]. First IMS experiments have been performed at the CSRe [73,74]. The masses of 63 Ge, 65 As and 67 Se and 71 Kr have been measured for the first time.…”

Section: Resultsmentioning

confidence: 99%

Mass and lifetime measurements of stored exotic nuclei

Litvinov¹,

Blaum²,

Winckler³

et al. 2011

Proceedings of 11th Symposium on Nuclei in the Cosmos — PoS(NIC XI)

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Knowledge of atomic masses is indispensable in nuclear structure and nuclear astrophysics. In the last two decades, majority of experimental data on nuclear masses stems from measurements of stored ions. The ions can be stored at low energies in a Penning trap or at significantly higher energies in a storage ring. In both cases revolution frequencies of ions trapped in a confining magnetic field are determined which enables high-precision mass measurements. In this contribution we sketch the experimental techniques and recent results. Future perspectives at the new generation radioactive beam facilities are outlined.

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Section: Resultsmentioning

confidence: 99%

Mass and lifetime measurements of stored exotic nuclei

Litvinov¹,

Blaum²,

Winckler³

et al. 2011

Proceedings of 11th Symposium on Nuclei in the Cosmos — PoS(NIC XI)

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“…If the experimental uncertainties could be further reduced to a smaller amount, say within ±150 keV, the result would be extremely significant. As pointed out by Xu et al [6] , this would change the current picture of the location of the proton drip-line, and strongly modify the so-far discussed results for the rp-process nucleosynthesis.…”

mentioning

confidence: 88%

“…The preliminary results for the measured masses presented in ref. [6] are interesting in that they would result in different conclusions as the prevalent believe. Unfortunately, the error bars prevent them from drawing an immediate conclusion.…”

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confidence: 99%

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Nuclear masses near the proton drip-line and their impact on nucleosynthesis in explosive stars

Sun

2009

Sci. Bull.

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The interplay of the fundamental forces (here mainly the strong force and electromagnetic force) holds nucleons together to form atomic nuclei. However, in nature only less than ten percent of the total number of nuclei is stable. The majority of nuclei are unstable; that is, after having lived for a certain time, they change into the daughter nuclei by radioactive decay. The familiar decay types that can be found in most parts of the chart of nuclide are α-decay and β-decay. There are other important processes in which unstable nuclei can change into other ones. These occur, for example, in very neutronrich or proton-rich regions of the chart of nuclide. There are boundaries called drip-lines, which are the lines on the Z (proton)-N (neutron) plane where the nucleon separation energy is zero. The nuclear binding becomes weaker and weaker when moving from the stable region towards the drip-lines, and eventually no nucleus can exist beyond the drip-lines. Taking the proton-rich region as an example, near the proton drip-line, protons are only weakly bound and a proton radioactivity can occur. Also because of the small binding, nuclei near the proton drip-line may capture additional protons and become new, heavier nuclides if the capture conditions are present. Detailed knowledge on the nucleon-capture processes lies at the heart of the understanding of nucleosynthesis in the Universe--a very fundamental but unanswered question about how the heavy elements (i.e. those heavier than iron) are created.In order for nuclei to capture protons, a high temperature environment (usually above 1×10 9 K) is needed so that they can overcome the large coulomb barrier for charged particle reactions. A hydrogen rich environment is also required to have a large proton flux [1] . The type-I X-ray bursts, which are explosive consequences of accreting neutron stars [2] , have been suggested to be the physical sites where the nucleosynthesis rp-process [3] (the rapid proton-capture process) takes place. The rpprocess consists of consecutive proton captures onto seed nuclei plus some β + -decays to produce new elements, which proceed in the proton-rich nuclei near the proton drip-line. Understanding the nucleosynthesis clearly requires a detailed analysis of the reaction path and the reaction flow in the whole mass range involved in the process. Particularly important for rp-process nuclear reaction network calculations are the nuclear masses of the proton-rich isotopes because these determine the Q values for proton-capture and β + -decay. Nuclear mass is such a sensitive and dominant quantity in the discussion that the quality and predictive power of the astrophysical models for nucleosynthesis depend crucially on the accuracy of the mass. However, only a very limited amount of experimental mass is presently available for proton-rich unstable nuclei with A>60 because of extreme difficulty in performing experiments in laboratory for such short-lived isotopes. Theoretical masses based on various mass model predictions are not reliable,...

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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].…”

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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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First mass measurement of short-lived nuclides at HIRFL-CSR

Cited by 23 publications

References 15 publications

Mass and lifetime measurements of stored exotic nuclei

Mass and lifetime measurements of stored exotic nuclei

Nuclear masses near the proton drip-line and their impact on nucleosynthesis in explosive stars

A new era of nuclear astrophysics research in China

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