Evidence for Radiogenic Sulfur-32 in Type AB Presolar Silicon Carbide Grains?

TL;DR

This study analyzes isotopic compositions of Type AB presolar silicon carbide grains, finding evidence that supports a born-again AGB star origin for grains with radiogenic sulfur-32, challenging previous supernova hypotheses.

Contribution

It provides new isotopic evidence linking Type AB grains with born-again AGB stars, offering an alternative to supernova origin theories.

Findings

Large 32S excesses observed in some grains.

Born-again AGB stars can produce 32Si, explaining 32S excesses.

Supernova origin for these grains is unlikely based on isotopic evidence.

Abstract

We report C, Si, and S isotope measurements on 34 presolar silicon carbide grains of Type AB, characterized by 12C/13C < 10. Nitrogen, Mg-Al-, and Ca-Ti-isotopic compositions were measured on a subset of these grains. Three grains show large 32S excesses, a signature that has been previously observed for grains from supernovae (SNe). Enrichments in 32S 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 32Si 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 44Ti, relatively low 26Al/27Al ratios (a few times 10-3), and radiogenic 32S along with low 12C/13C 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 12C/13C ratios and enhanced abundances of the light s-process elements, can produce 32Si, which makes such stars attractive sources for AB grains with 32S 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.