The neutron capture process in the He shell in core-collapse supernovae: Presolar silicon carbide grains as a diagnostic tool for nuclear astrophysics

1,2Marco Pignatari, 3Peter Hoppe, 4,2Reto Trappitsch, 5,2Chris Fryer, 6,7,2F.X. Timmes, 8,9,2Falk Herwig, 9,10,2Raphael Hirschi
Geochmica et Cosmochimica Acta (in Press) Link to Article []
1E. A. Milne Centre for Astrophysics, University of Hull, Hull, HU6 7RX, UK
2The NuGrid Collaboration (
3Max Planck Institute for Chemistry, Hahn-Meitner-Weg 1, 55128 Mainz, Germany
4Department of the Geophysical Sciences, The University of Chicago, and Chicago Center for Cosmochemistry, Chicago, IL 60637, USA
5Computational Physics and Methods (CCS-2), LANL, Los Alamos, NM, 87545, USA
6Arizona State University (ASU), PO Box 871404, Tempe, AZ, 85287-1404, USA
7The Joint Institute for Nuclear Astrophysics, Notre Dame, IN 46556, USA
8Department of Physics & Astronomy, University of Victoria, Victoria, BC, V8P5C2 Canada
9Keele University, Keele, Staffordshire ST5 5BG, United Kingdom
10Institute for the Physics and Mathematics of the Universe (WPI), University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa 277-8583, Japan
Copyright Elsevier

Carbon-rich presolar grains are found in primitive meteorites, with isotopic measurements to date suggesting a core-collapse supernovae origin site for some of them. This holds for about 1-2 % of presolar silicon carbide (SiC) grains, so-called Type X and C grains, and about 30 % of presolar graphite grains. Presolar SiC grains of Type X show anomalous isotopic signatures for several elements heavier than iron compared to the solar abundances: most notably for strontium, zirconium, molybdenum, ruthenium and barium. We study the nucleosynthesis of zirconium and molybdenum isotopes in the He-shell of three core-collapse supernovae models of 15, 20 and 25 M☉ with solar metallicity, and compare the results to measurements of presolar grains. We find the stellar models show a large scatter of isotopic abundances for zirconium and molybdenum, but the mass averaged abundances are qualitatively similar to the measurements. We find all models show an excess of 96Zr relative to the measurements, but the model abundances are affected by the fractionation between Sr and Zr since a large contribution to 90Zr is due to the radiogenic decay of 90Sr. Some supernova models show excesses of 95,97Mo and depletion of 96Mo relative to solar. The mass averaged distribution from these models shows an excess of 100Mo, but this may be alleviated by very recent neutron-capture cross section measurements. We encourage future explorations to assess the impact of the uncertainties in key neutron-capture reaction rates that lie along the n-process path.


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