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Pre-solar grains from supernovae and novae

Published online by Cambridge University Press:  01 August 2006

Sachiko Amari  and
Katharina Lodders
Sachiko Amari
Affiliation:
Laboratory for Space Sciences & the Physics Department
Katharina Lodders
Affiliation:
Department of Earth and Planetary Sciences, Washington University, St. Louis, MO 63130, USA email: sa@wuphys.wustl.edu, lodders@wustl.edu
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Abstract

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Pre-solar grains from supernova ejecta – silicon carbide of type X, Si3N4 and low-density graphite – are characterized by Si isotopic anomalies (mainly 28Si excesses), low 14N/15N, high 26Al/27 Al ratios, and occasionally by excesses in 44Ca (from 44Ti decay). Overall isotopic features of these SiC and graphite grains can be explained by mixing of inner Si-rich zones and the outer C-and He-rich zones, but supernova models require fine tuning to account for 14N/15N and 29Si/28Si ratios of the grains. Isotopic ratios of Zr, Mo and Ba in SiC X grains may be explained by a neutron burst model. Some of the pre-solar nanodiamonds require a supernova origin to explain measured xenon isotopic ratios. Only a few nova grain candidates, with low 12C/13C, 14N/15N, and high 26Al/27 Al ratios, have been identified.

Keywords

meteorsmeteoroidsstars: supernovae: generalstars: novaecataclysmic variables
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 2 , Highlights of Astronomy 14: Highlights of Astronomy , August 2006 , pp. 349 - 352
Copyright
Copyright © International Astronomical Union 2007

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