Production of carbon-rich presolar grains from massive stars

M. Pignatari, M. Wiescher, Francis Timmes, R. J. De Boer, F. K. Thielemann, C. Fryer, A. Heger, F. Herwig, R. Hirschi

Research output: Contribution to journalArticle

26 Citations (Scopus)

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 12C(α, γ)16O reaction relative to the rest of the α-capture chain at T > 3.5 × 108 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 44Ca/40Ca observed in the grains. This is due to the production of 44Ti together with 40Ca in the C/Si zone and/or to the strong depletion of 40Ca by neutron captures.

Original languageEnglish (US)
Article numberL22
JournalAstrophysical Journal Letters
Volume767
Issue number2
DOIs
StatePublished - Apr 20 2013

Fingerprint

massive stars
supernovae
silicon
explosive
carbon
shell
nuclear fusion
prediction
isotopic ratio
ejecta
meteorite
explosion
dust
meteorites
oxygen
predictions
silicon carbides
explosions
depletion
shock

Keywords

  • stars: abundances
  • stars: evolution
  • stars: interiors

ASJC Scopus subject areas

  • Space and Planetary Science
  • Astronomy and Astrophysics

Cite this

Pignatari, M., Wiescher, M., Timmes, F., De Boer, R. J., Thielemann, F. K., Fryer, C., ... Hirschi, R. (2013). Production of carbon-rich presolar grains from massive stars. Astrophysical Journal Letters, 767(2), [L22]. https://doi.org/10.1088/2041-8205/767/2/L22

Production of carbon-rich presolar grains from massive stars. / Pignatari, M.; Wiescher, M.; Timmes, Francis; De Boer, R. J.; Thielemann, F. K.; Fryer, C.; Heger, A.; Herwig, F.; Hirschi, R.

In: Astrophysical Journal Letters, Vol. 767, No. 2, L22, 20.04.2013.

Research output: Contribution to journalArticle

Pignatari, M, Wiescher, M, Timmes, F, De Boer, RJ, Thielemann, FK, Fryer, C, Heger, A, Herwig, F & Hirschi, R 2013, 'Production of carbon-rich presolar grains from massive stars', Astrophysical Journal Letters, vol. 767, no. 2, L22. https://doi.org/10.1088/2041-8205/767/2/L22
Pignatari M, Wiescher M, Timmes F, De Boer RJ, Thielemann FK, Fryer C et al. Production of carbon-rich presolar grains from massive stars. Astrophysical Journal Letters. 2013 Apr 20;767(2). L22. https://doi.org/10.1088/2041-8205/767/2/L22
Pignatari, M. ; Wiescher, M. ; Timmes, Francis ; De Boer, R. J. ; Thielemann, F. K. ; Fryer, C. ; Heger, A. ; Herwig, F. ; Hirschi, R. / Production of carbon-rich presolar grains from massive stars. In: Astrophysical Journal Letters. 2013 ; Vol. 767, No. 2.
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