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

Wasserburg, G. J. and Busso, M. and Gallino, R. and Nollett, K. M. (2006) Short-lived nuclei in the early Solar System: Possible AGB sources. Nuclear Physics A, 777 . pp. 5-69. ISSN 0375-9474. https://resolver.caltech.edu/CaltechAUTHORS:20131120-090059030

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Abstract

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)CI, ^(26)AI, 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)CI. Both of these nuclei appear to be present when ^(26)AI 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 ƒ_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)CI if it is very abundant. The role of irradiation is discussed with regard to ^(26)AI, ^(36)CI 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 yr 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.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://arxiv.org/abs/astro-ph/0602551arXivDiscussion Paper
http://dx.doi.org/10.1016/j.nuclphysa.2005.07.015DOIArticle
http://www.sciencedirect.com/science/article/pii/S037594740501002XPublisherArticle
Additional Information:© 2005 Elsevier B.V. Received 8 March 2005; received in revised form 11 July 2005; accepted 12 July 2005. Available online 11 August 2005. The authors thank the editors for their indulgence in handling this tardy submission of a very long report. The efforts of Uli Ott in providing a detailed, thorough, incisive and scholarly review have greatly improved this work. Extremely useful comments and criticisms were provided by Ian Hutcheon as well as a possible but thankfully not realized SNe shock. We are indebted to useful comments by F. Käppeler, J. Truran, A. McKeegan, A. Davis and M. Thiemens, as well as several other colleagues. M.E. Johnson did her usual superior work in cryptography and a special effort in re-encoding on the many versions of this manuscript. M.B. and R.G. acknowledge financial support in Italy by MIUR, under contract PRIN2004-025729. G.J.W. acknowledges the support of DOE-DE-FG03-88ER13851. K.M.N. was supported by the US DOE, Nuclear Physics Division, under contract No. W-31-109-ENG-38. Caltech Division Contribution 9014(1119).
Funders:
Funding AgencyGrant Number
Multidisciplinary University Research Initiative (MURI) ItalyPRIN2004-025729
Department of Energy (DOE)DE-FG03-88ER3851
Department of Energy (DOE) Nuclear Physics DivisionW-31-109-ENG-38
Subject Keywords:Solar abundances; Short-lived nuclei; Nucleosynthesis; Solar System formation; Isotopic anomalies; Stars, AGB; Stars, Supernovae
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Caltech Division of Geological and Planetary Sciences9014
Lunatic Asylum Lab1119
Record Number:CaltechAUTHORS:20131120-090059030
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20131120-090059030
Official Citation:G.J. Wasserburg, M. Busso, R. Gallino, K.M. Nollett, Short-lived nuclei in the early Solar System: Possible AGB sources, Nuclear Physics A, Volume 777, 17 October 2006, Pages 5-69, ISSN 0375-9474, http://dx.doi.org/10.1016/j.nuclphysa.2005.07.015. (http://www.sciencedirect.com/science/article/pii/S037594740501002X)
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:42584
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:20 Nov 2013 21:46
Last Modified:03 Oct 2019 05:59

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