Neutron-capture nucleosynthesis in the helium-burning cores of massive stars

Lamb, S. A.; Howard, W. M.; Truran, J. W.; Iben, Icko

doi:10.1086/155571

Cited by 132 publications

(77 citation statements)

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“…While B 2 FH correctly surmised that the bulk of the Fe-group isotopes in the solar system were made in equilibrium processes, they also found that the s process had to be responsible for the synthesis of some of the iron-group nuclides. Work since 1957 has confirmed this to be the case (e.g., Peters et al, 1972;Lamb et al, 1977;Baraffe et al, 1992). In this process, seed iron-group nuclei from previous generations of stars are exposed to a flux of neutrons.…”

Section: A Brief History Of the Ideas Of Iron-group Element Synthesismentioning

confidence: 90%

“…Combining the Schrö der et al (1987) measurements with the earlier low-energy (93ϽE c.m. Ͻ126 keV) measurements of Lamb and Hester (1957), determines S(0)=3.5 Ϫ1.6 +0.4 keV b (INT Workshop, 1997), where the uncertainty arises primarily from uncertainty (because of the interference effects due to the subthreshold resonance) in how to extrapolate the laboratory measurements to zero energy. This uncertainty in the rate of the 14 N(p,␥) 15 O reaction corresponds to an uncertainty of ϳ1 Gy in the age of globular clusters (e.g., Chaboyer et al, 1996;.…”

Section: Hydrogen Burning In the Pp Chain And Cn Cyclementioning

confidence: 99%

“…The weak component has been ascribed to core helium burning in massive stars (Peters, 1968;Couch, Schmeidekamp, and Arnett, 1974;Lamb et al, 1977;Langer et al, 1989;El Eid and Baraffe, 1990; when the temperatures become sufficiently high for neutron production via the 22 Ne(␣,n) 25 Mg reaction. The resulting neutron density is comparatively low and lasts for about 3ϫ10 4 yr, resulting in the modest neutron exposure of the weak s-process component.…”

Section: The N Curvementioning

confidence: 99%

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Synthesis of the elements in stars: forty years of progress

et al. 1997

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Forty years ago Burbidge, Burbidge, Fowler, and Hoyle combined what we would now call fragmentary evidence from nuclear physics, stellar evolution and the abundances of elements and isotopes in the solar system as well as a few stars into a synthesis of remarkable ingenuity. Their review provided a foundation for forty years of research in all of the aspects of low energy nuclear experiments and theory, stellar modeling over a wide range of mass and composition, and abundance studies of many hundreds of stars, many of which have shown distinct evidence of the processes suggested by B 2 FH. In this review we summarize progress in each of these fields with emphasis on the most recent developments. [S0034-6861(97)

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Section: A Brief History Of the Ideas Of Iron-group Element Synthesismentioning

confidence: 90%

Section: Hydrogen Burning In the Pp Chain And Cn Cyclementioning

confidence: 99%

Section: The N Curvementioning

confidence: 99%

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Synthesis of the elements in stars: forty years of progress

et al. 1997

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“…The light neutron-capture elements Sr, Y, and Zr are thought to be significantly produced in the weak s-process, which has been proposed to occur in advanced evolutionary phases of massive (M > 10 M ) stars (Lamb et al 1977). Because these elements are produced in massive stars, they should be overabundant at early epochs, although because the weak s-process elements' production has been suggested to depend on metallicity (Raiteri et al 1992), the overabundance may not be as great as that of the r-process elements.…”

Section: Heavy Elementsmentioning

confidence: 99%

A Comparison of the Chemical Evolutionary Histories of the Galactic Thin Disk and Thick Disk Stellar Populations

Brewer

Carney

2006

Astron J

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We have studied 23 long-lived G dwarfs that belong to the thin disk and thick disk stellar populations. The stellar data and analyses are identical, reducing the chances for systematic errors in the comparisons of the chemical abundance patterns in the two populations. Other elements share this same behavior, including Sc, Co, and Zn, suggesting that at least in the chemical enrichment history of the thick disk, these elements were manufactured in similar-mass stars. The heavy s-process elements Ba, La, Ce, and Nd are overabundant in the thin disk stars relative to the thick disk stars. On the other hand, the constancy of the [Ba /Y ] ratio suggests that only one s-process site was manufacturing these elements or, possibly, that the r-process was responsible for the bulk of the nucleosynthesis of these elements. We combine our results with other studies (Edvardsson et al., Prochaska et al., Bensby et al., and Reddy et al.), who had already found very similar trends, in order to further explore the origin of the thick disk. The signs for an independent (parent galaxy) evolution of the thick

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“…The weak component of the astrophysical s process observed in the solar system abundance distribution includes the s-process species between Fe and Sr (60 < A < 90) [1]. Most of them are generated in massive stars during convective He core burning and convective C shell burning via the activation of the neutron source reaction 22 Neð ; nÞ 25 Mg [2][3][4][5][6]. The long-lived radioisotope 63 Ni (t 1=2 ¼ 101:2 AE 1:5 yr [7]) is located along the neutron capture path, and in typical weak s-process conditions it may become a branching point, when the neutron capture time scale is comparable with its stellar -decay rate.…”

mentioning

confidence: 99%