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Short-Lived Nuclei in the Early Solar System: A Low Mass Stellar Source?

Busso, M. and Gallino, R. and Wasserburg, G. J. (2003) Short-Lived Nuclei in the Early Solar System: A Low Mass Stellar Source? Publications of the Astronomical Society of Australia, 20 (4). pp. 356-370. ISSN 1323-3580. https://resolver.caltech.edu/CaltechAUTHORS:20131119-090812510

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Abstract

We discuss possible stellar origins of short-lived radioactive nuclei with meanlife τ ≤ 100 Myr, which were shown to be alive in the Early Solar System (ESS). We first review current ideas on the production of nuclides having 10 ≤ τ ≤ 100 Myr, which presumably derive from the continuous interplay of galactic astration, nucleosynthesis from massive supernovae and free decay in the interstellar medium. The abundance of the shorter lived ^(53)Mn might be explained by this same scenario. Then we consider the nuclei ^(107)Pd, ^(26)Al, ^(41)Ca and ^(60)Fe, whose early solar system abundances are too high to have originated in this way. Present evidence favours a stellar origin, particularly for ^(107)Pd, ^(26)Al and ^(60)Fe, rather than an in situ production by energetic solar particles. The idea of an encounter (rather close in time and space) between the forming Sun and a dying star is therefore discussed: this star may or may not have also triggered the solar formation. Recent nucleosynthesis calculations for the yields of the relevant short-lived isotopes and of their stable reference nuclei are discussed. Massive stars evolving to type II supernovae (either leaving a neutron star or a black hole as a remnant) seem incapable of explaining the four most critical ESS radioactivities in their observed abundance ratios. An asymptotic giant branch (AGB) star seems to be a viable source, especially if of relatively low initial mass (M ≤ 3 M_⊙) and with low neutron exposure: this model can provide a solution for ^(26)Al, ^(41)Ca and ^(107)Pd, with important contributions to ^(60)Fe, which are inside the present uncertainty range of the ^(60)Fe early solar system abundance. Such a model requires that ^(26)Al is produced substantially on the AGB by cool bottom processing. The remaining inventory of short-lived species in the solar nebula would then be attributed to the continuous galactic processing, with the exception of ^(10)Be, which must reflect production by later proton bombardment at a low level during early solar history.


Item Type:Article
Related URLs:
URLURL TypeDescription
http://dx.doi.org/10.1071/AS03035DOIArticle
http://journals.cambridge.org/action/displayAbstract?fromPage=online&aid=8839666PublisherArticle
Additional Information:© 2003 Astronomical Society of Australia. Received 2003 May 4, accepted 2003 July 4. We all wish to thank John Lattanzio for his generous share of information, data, advice and good wines. Suggestions of critical importance and stimulating comments were provided by G. Lugmair, E. Zinner, J. José, O. Straniero, M. Limongi and A. Chieffi. In particular, we would like to acknowledge the extremely helpful and detailed comments and criticisms by G. Huss that greatly aided in improving this report. Cynthia A. Craig reminded us old Italian aphorisms, which are useful in a wide variety of occasions. M.B. and R.G. acknowledge support from the Italian MIUR-FIRB Project M_⊙ ‘Astrophysical Origin of Heavy Elements beyond Fe’. G.J.W. acknowledges support from NASA NAGS-11725. Caltech Division Contribution 8905(1107).
Funders:
Funding AgencyGrant Number
MIUR-FIRB UNSPECIFIED
NASANAGS-11725
Subject Keywords: solar system: formation; stars: AGB and post-AGB; stars: supernovae: general
Other Numbering System:
Other Numbering System NameOther Numbering System ID
Caltech Division of Geological and Planetary Sciences 8905
Lunatic Asylum Lab1107
Issue or Number:4
Record Number:CaltechAUTHORS:20131119-090812510
Persistent URL:https://resolver.caltech.edu/CaltechAUTHORS:20131119-090812510
Official Citation: M. Busso, R. Gallino and G. J. Wasserburg (2003). Short-Lived Nuclei in the Early Solar System: A Low Mass Stellar Source?. Publications of the Astronomical Society of Australia, 20, pp 356-370. doi:10.1071/AS03035.
Usage Policy:No commercial reproduction, distribution, display or performance rights in this work are provided.
ID Code:42553
Collection:CaltechAUTHORS
Deposited By: Ruth Sustaita
Deposited On:19 Nov 2013 17:28
Last Modified:03 Oct 2019 05:59

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