Measurement and Analysis of 98Mo(n,γ)99Mo Reaction Cross Section

Chunhao, Wang; Yijun, Xia; Long, Xiaojiang; Jingfu, Yang; Yang, Zhihua; Peng, Xiufeng; Liu, Mantian; Lu, Haijiao

doi:10.1007/978-3-642-58113-7_108

Cited by 5 publications

(34 citation statements)

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“…Accurate values of cross sections for them are necessary to eliminate the discrepancies with the isotopic anomalies, i.e., the isotopic ratios of Kr isotopes. For example, a large spread in the ratio of 86 Kr to 82 Kr with the size of grains found in SiC is a longstanding problem in AGB star model of s-process.…”

Section: B Total Capture Cross Sectionsmentioning

confidence: 99%

“…At this point, the flow of mass depends on neutron density, i.e., for a sufficiently high neutron density, the neutron channel is open and a competition takes place between β-decay and neutron capture. The ground state β-decay half-life, which stays constant with temperature, becomes long enough so that the s-process path feeds 86 Kr via neutron capture and afterward the path moves towards 87 Rb. It is also possible to the measure the isomeric ratio of 85 Kr if both total 87 Rb is of special interest as 86 Kr is a closed neutron shell nucleus having comparatively lower cross sections and hence acts as a waiting point in the reaction chain.…”

Section: B Total Capture Cross Sectionsmentioning

confidence: 99%

“…They are considered to be produced in both main and weak components of stellar s-process nucleosynthesis. For example, 50% of the solar abundances of the s-only pair 86,87 The present study also involves some nuclei produced in astrophysical p-process near N = 50 closed shell ( 84 Sr, 92,94 Mo, 96,98 Ru). The p-nuclei, those are 10 to 100 times less abundant than s-or r-nuclei in the same mass range are produced in the high-temperature environment via the sequences of photo-disintegration and β + decays driving the path through the extreme proton-rich side.…”

Section: Introductionmentioning

confidence: 99%

“…They are considered to be produced in both main and weak components of stellar s-process nucleosynthesis. For example, 50% of the solar abundances of the s-only pair 86,87 Sr are formed in the main component and remaining 50% are from the weak component of sprocess [4]. In the concerned mass region, there are six stable nuclei on the nucleosynthesis path with magic neutron number N = 50, namely, 86 Kr, 87 Rb, 88 Sr, 89 Y, and 90 Zr, and 92 Mo.…”

Section: Introductionmentioning

confidence: 99%

“…In Figs. 3 and 4, we plot the experimental and calculated cross sections of 80,82,83,84,86 Kr as well as 85,87 Rb. Isotopes of krypton are of special interest as they can give valuable information for s-process nucleosynthesis study.…”

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confidence: 99%

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Neutron capture reactions relevant to thesandpprocesses in the region of theN=50shell closure

2016

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Radiative thermal neutron capture cross sections for nuclei participating in s-process and pprocess nucleosynthesis in and around N = 50 closed neutron shell have been calculated in statistical semi-microscopic Hauser-Feshbach approach for the energy range of astrophysical interest. A folded optical-model potential is constructed utilizing the standard DDM3Y real nucleon-nucleon interaction. The folding of the interaction with target radial matter densities, obtained from the relativistic-mean-field approach, is done in coordinate space using the spherical approximation. The standard nuclear reaction code TALYS1.8 is used for cross-section calculation. The cross sections are compared with experimental results and reasonable agreements are found for almost all cases. Maxwellian-averaged cross sections (MACS) for the nuclei are presented at a single thermal energy of 30 keV relevant to s-process. We have also presented the MACS values over a range of energy from 5 to 100 keV for neutron magic nuclei with (N = 50).PACS numbers: I. INTRODUCTIONElements heavier than iron are produced via two principle processes, namely, the slow neutron capture process (s-process) and the rapid neutron capture process (r-process), differing in the respective neutron capture timescales with respect to the β-decay half-lives. There is a minor contribution from another process, namely, pprocess, producing a subset of proton-rich isotopes. The detailed study of the heavy element nucleosynthesis was done in the fundamental work of Burbidge et al. [1] and also of Cameron [2]. Recently Käppeler et al. [3] presented a review of progress on the studies of s-process nucleosynthesis with advanced nuclear physics inputs, observational data, and stellar models.While the majority of the theory of the s-process is well-developed, uncertainty still remains in constraining the neutron capture rates of nuclei involved in nucleosynthesis chain. The capture cross sections are highly scattered and uncertain in the energy range appropriate for astrophysical applications. These uncertainties lead to significant errors in determining exact abundances of elements involved in different processes. Many works * Electronic address: saumidutta89@gmail.com † Electronic address: ggphy@caluniv.ac.in ‡ Electronic address: abhattacharyyacu@gmail.com have been devoted to this respect in order to measure the thermal neutron capture cross sections relevant to s-process temperature. However, reactions on some important nuclei are still not available due to their unavailability in the terrestrial laboratory. Käppeler et al. [4] showed the present status of the uncertainty of stellar (n, γ) cross sections and commented that improvements are certainly necessary especially in the mass region below A=120 and above A=180. Some reactions are of significant importance, basically those with closed neutron shells acting as bottlenecks to the s-process reaction flow. They have very low cross-sections and in some scenarios, the s-process reaction flow cannot overcome these bottlen...

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Section: B Total Capture Cross Sectionsmentioning

confidence: 99%