Live Iron-60 in the Early Solar System

Shukolyukov, A.; Lugmair, G. W.

doi:10.1126/science.259.5098.1138

Cited by 161 publications

(120 citation statements)

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“…The MS and S stars have been studied by Smith and Lambert (1990), Plez et al (1993), Busso et al (1995), and , while the most detailed analysis of the s process in the carbon stars is still Utsumi (1985). Recent abundance studies have uncovered s-process rich post-AGB stars in the globular cluster Cen (Gonzalez and Wallerstein, 1994), as well as s-process enhancements in the yellow symbiotics (Smith et al, , 1997.…”

Section: B Observations Of Nucleosynthesis and Mixing In Ch Ba S mentioning

confidence: 99%

“…In addition, it has been shown that the 40% of S stars which do not show the lines of Tc I in their spectra are the cooler relatives of the Ba stars and result from mass transfer Smith and Lambert, 1988;Brown et al, 1990;Jorissen et al, 1993). Most recently, a number of the active symbiotic binaries have been identified as C rich (Schmid and Nussbaumer, 1993;Schmid, 1994), while the yellow symbiotic stars AG Dra and BD-21°3873 have both been shown to be s-process rich and thus technically Ba stars as well as symbiotics (Smith et al, , 1997. There is now a coherent picture of the s-process rich classes of stars: the N-type carbon stars, along with the MS and S stars with Tc, are bonafide AGB stars that have recently dredged fresh s-process material to their surfaces.…”

Section: B Observations Of Nucleosynthesis and Mixing In Ch Ba S mentioning

confidence: 99%

“…In the last 15 years or so a number of results for Rb have become available for Ba stars (Tomkin and Lambert, 1983;Smith and Lambert, 1984;Malaney and Lambert, 1988), the MS and S stars , s-process rich giants in the globular cluster Cen (Vanture et al, 1994), and the s-process rich yellow symbiotic stars (Smith et al, , 1997. In addition, Wallerstein (1992) has analyzed the Rb I resonance line in emission in the S star, R Andromeda, and estimated the Rb/K abundance ratio (using the K I resonance line also in emission).…”

Section: Rubidium and The S-process Neutron Densitymentioning

confidence: 99%

“…Because the temperature and density vary throughout the radiative He shell, each radiative layer is characterized by different conditions, such that the resulting distribution of neutron exposures is not an exponential distribution. Further modeling may result in bet-ter fits to the abundance distributions in low metallicity s-process rich stars which, traditionally, seem to have been better fit by single exposure models (e.g., Vanture, 1992a;Smith et al, 1996Smith et al, , 1997.…”

Section: Rubidium and The S-process Neutron Densitymentioning

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: B Observations Of Nucleosynthesis and Mixing In Ch Ba S mentioning

confidence: 99%

Section: B Observations Of Nucleosynthesis and Mixing In Ch Ba S mentioning

confidence: 99%

Section: Rubidium and The S-process Neutron Densitymentioning

confidence: 99%

Section: Rubidium and The S-process Neutron Densitymentioning

confidence: 99%

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Synthesis of the elements in stars: forty years of progress

et al. 1997

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“…The hints of 60 Fe (τ = 2.2 Myr) discovered by Shukolyukov & Lugmair [42] [43] and the subsequent recent demonstration of 60 Ni excesses correlated with Fe/Ni in chondrites, require 60 Fe to be present at rather high abundances in the early solar system [44] [45] [46]. This nucleus has connections to both supernovae and asymptotic giant branch (AGB) sources, but not to spallation reactions.…”

Section: Introductionmentioning

confidence: 99%

Short-lived nuclei in the early Solar System: Possible AGB sources

et al. 2006

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The abundances of short-lived radionuclides in the early solar system (ESS) are reviewed, as well as the methodology used in determining them. These results are compared with the inventory estimated for a uniform galactic production model. It is shown that, to within a factor of two, the observed abundances of 238 U, 235 U, 232 Th, 244 Pu, 182 Hf, 146 Sm, and 53 Mn are roughly compatible with long-term galactic nucleosynthesis. 129 I is an exception, with an ESS inventory much lower than expected from uniform production. The isotopes 107 Pd, 60 Fe, 41 Ca, 36 Cl, 26 Al, and 10 Be require late addition to the protosolar nebula. 10 Be is the product of energetic particle irradiation of the solar system as most probably is 36 Cl. Both of these nuclei appear to be present when 26 Al is absent. A late injection by a supernova (SN) cannot be responsible for most of the short-lived nuclei without excessively producing 53 Mn; it can however be the source of 53 Mn itself and possibly of 60 Fe. If a late SN injection is responsible for these two nuclei, then there remains the problem of the origin of 107 Pd and several other isotopes. Emphasis is given to an AGB star as a source of many of the nuclei, including 60 Fe; this possibility is explored with a new generation of stellar models. It is shown that if the dilution factor (i.e. the ratio of the contaminating mass to the solar parental cloud mass) is f 0 ∼ 4×10 −3 , a reasonable representation for many nuclei is obtained; this requires that ( 60 Fe/ 56 Fe) ESS ∼ 10 −7 to 2×10 −6 . The nuclei produced by an AGB source do not include 53 Mn, 10 Be or 36 Cl if it is very abundant. The role of irradiation is discussed with regard to 26 Al, 36 Cl and 41 Ca, and the estimates of bulk solar abundances of these isotopes are commented on. The conflict between various scenarios is emphasized as well as the current absence of an astrophysically plausible global interpretation for all the existing data. Examination of abundances for the actinides indicates that a quiescent interval of ∼ 10 8 years is required for actinide group production. This is needed in order to explain the data on 244 Pu and the new bounds on 247 Cm. Because this quiescent interval is not compatible with the 182 Hf data, a separate type of r-process event is needed for at least the actinides, distinct from the two types that have previously been identified. The apparent coincidence of the 129 I and trans-actinide time scales suggests that the last heavy r contribution was from an r-process that produced very heavy nuclei but without fission recycling so that the yields at Ba and below (including I) were governed by fission.

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Gravitational Deformation in Shaping Asteroids and Small Satellites

Slyuta

Воропаев

1997

Icarus

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Live Iron-60 in the Early Solar System

Cited by 161 publications

References 23 publications

Synthesis of the elements in stars: forty years of progress

Synthesis of the elements in stars: forty years of progress

Short-lived nuclei in the early Solar System: Possible AGB sources

Gravitational Deformation in Shaping Asteroids and Small Satellites

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