Home News About Us Contact Contributors Disclaimer Privacy Policy Help FAQ

Home
Search
Quick Search
Advanced
Fulltext
Browse
Collections
Persons
My eDoc
Session History
Login
Name:
Password:
Documentation
Help
Support Wiki
Direct access to
document ID:


          Institute: MPI für Chemie     Collection: Publikationen MPI für Chemie     Display Documents



ID: 675659.0, MPI für Chemie / Publikationen MPI für Chemie
Evidence for Radiogenic Sulfur-32 in Type AB Presolar Silicon Carbide Grains?
Authors:Fujiya, W.; Hoppe, P.; Zinner, E.; Pignatari, M.; Herwig, F.
Language:English
Date of Publication (YYYY-MM-DD):2013-10-20
Title of Journal:Astrophysical Journal Letters
Volume:776
Issue / Number:2
Sequence Number of Article:L29
Review Status:Internal review
Audience:Experts Only
Abstract / Description:We report C, Si, and S isotope measurements on 34 presolar silicon carbide grains of Type AB, characterized by C-12/C-13 < 10. Nitrogen, Mg-Al-, and Ca-Ti-isotopic compositions were measured on a subset of these grains. Three grains show large S-32 excesses, a signature that has been previously observed for grains from supernovae (SNe). Enrichments in S-32 may be due to contributions from the Si/S zone and the result of S molecule chemistry in still unmixed SN ejecta or due to incorporation of radioactive Si-32 from C-rich explosive He shell ejecta. However, a SN origin remains unlikely for the three AB grains considered here, because of missing evidence for Ti-44, relatively low Al-26/Al-27 ratios (a few times 10(-3)), and radiogenic S-32 along with low C-12/C-13 ratios. Instead, we show that born-again asymptotic giant branch (AGB) stars that have undergone a very-late thermal pulse (VLTP), known to have low C-12/C-13 ratios and enhanced abundances of the light s-process elements, can produce Si-32, which makes such stars attractive sources for AB grains with S-32 excesses. This lends support to the proposal that at least some AB grains originate from born-again AGB stars, although uncertainties in the born-again AGB star models and possible variations of initial S-isotopic compositions in the parent stars of AB grains make it difficult to draw a definitive conclusion.
External Publication Status:published
Document Type:Article
Version Comment:Automatic journal name synchronization
Communicated by:N. N.
Affiliations:MPI für Chemie
Identifiers:ISI:000325490200012 [ID No:1]
ISSN:2041-8205 [ID No:2]
The scope and number of records on eDoc is subject to the collection policies defined by each institute - see "info" button in the collection browse view.