Production of carbon-rich presolar grains from massive stars

Abstract

About a year after core collapse supernova, dust starts to condense in the ejecta. In meteorites, a fraction of C-rich presolar grains (e.g., silicon carbide (SiC) grains of Type-X and low density graphites) are identified as relics of these events, according to the anomalous isotopic abundances. Several features of these abundances remain unexplained and challenge the understanding of core-collapse supernovae explosions and nucleosynthesis. We show, for the first time, that most of the measured C-rich grain abundances can be accounted for in the C-rich material from explosive He burning in core-collapse supernovae with high shock velocities and consequent high temperatures. The inefficiency of the ${}^{12}$C($\alpha$,$\gamma$)${}^{16}$O reaction relative to the rest of the $\alpha$-capture chain at $T>3.5\times 10^8\mathrm{K}$ causes the deepest He-shell material to be carbon rich and silicon rich, and depleted in oxygen. The isotopic ratio predictions in part of this material, defined here as the C/Si zone, are in agreement with the grain data. The high-temperature explosive conditions that our models reach at the bottom of the He shell, can also be representative of the nucleosynthesis in hypernovae or in the high-temperature tail of a distribution of conditions in asymmetric supernovae. Finally, our predictions are consistent with the observation of large ${}^{44}$Ca/${}^{40}$Ca observed in the grains. This is due to the production of ${}^{44}$Ti together with ${}^{40}$Ca in the C/Si zone, and/or to the strong depletion of ${}^{40}$Ca by neutron captures.

13 pages, 4 figures, The Astrophysical Journal Letters, accepted

References in corpus (2)

• Compact Remnant Mass Function: Dependence on the Explosion Mechanism and Metallicity
• The effect of 12C + 12C rate uncertainties on the evolution and nucleosynthesis of massive stars

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