Presolar Silicon Carbide Grains of Types Y and Z: Their Molybdenum Isotopic Compositions and Stellar Origins

Liu, Nan; Stephan, Thomas; Cristallo, Sergio; Gallino, Roberto; Boehnke, Patrick; Nittler, Larry R.; Alexander, Conel M. O’D.; Davis, Andrew M.; Trappitsch, Reto; Pellin, Michael J.; Dillmann, Iris

doi:10.3847/1538-4357/ab2d27

Title: Presolar Silicon Carbide Grains of Types Y and Z: Their Molybdenum Isotopic Compositions and Stellar Origins

Journal Article · Fri Aug 09 00:00:00 EDT 2019 · The Astrophysical Journal (Online)

DOI:https://doi.org/10.3847/1538-4357/ab2d27· OSTI ID:1571732

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^[4]; Boehnke, Patrick ^[2];

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Washington Univ. in St. Louis, St. Louis, MO (United States); Carnegie Inst. for Science, Washington, D.C. (United States)
The Univ. of Chicago, Chicago, IL (United States); Chicago Center for Cosmochemistry, Chicago, IL (United States)
INAF-Osservatorio Astronomico d’Abruzzo, Teramo (Italy); INFN-Sezione di Perugia, Perugia (Italy)
Univ. di Torino, Torino (Italy)
Carnegie Inst. for Science, Washington, D.C. (United States)
The Univ. of Chicago, Chicago, IL (United States); Chicago Center for Cosmochemistry, Chicago, IL (United States); Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)
The Univ. of Chicago, Chicago, IL (United States); Chicago Center for Cosmochemistry, Chicago, IL (United States); Argonne National Lab. (ANL), Argonne, IL (United States)
TRIUMF, Vancouver, BC (Canada); Univ. of Victoria, BC (Canada)

We report Mo isotopic compositions of 37 presolar SiC grains of types Y (19) and Z (18), rare types commonly argued to have formed in lower-than-solar metallicity asymptotic giant branch (AGB) stars. Here direct comparison of the Y and Z grain data with data for mainstream grains from AGB stars of close-to-solar metallicity demonstrates that the three types of grains have indistinguishable Mo isotopic compositions. We show that the Mo isotope data can be used to constrain the maximum stellar temperatures (T _MAX) during thermal pulses in AGB stars. Comparison of FRUITY Torino AGB nucleosynthesis model calculations with the grain data for Mo isotopes points to an origin from low-mass (~1.5–3 M _⊙) rather than intermediate-mass (>3–~9 M _⊙) AGB stars. Because of the low efficiency of ²²Ne(α, n)²⁵Mg at the low T MAX values attained in low-mass AGB stars, model calculations cannot explain the large ³⁰Si excesses of Z grains as arising from neutron capture, so these excesses remain a puzzle at the moment.

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Research Organization:: Lawrence Livermore National Lab. (LLNL), Livermore, CA (United States)

Sponsoring Organization:: USDOE National Nuclear Security Administration (NNSA)

Grant/Contract Number:: AC52-07NA27344

OSTI ID:: 1571732

Report Number(s):: LLNL-JRNL-765107; 955089; TRN: US2100331

Journal Information:: The Astrophysical Journal (Online), Vol. 881, Issue 1; ISSN 1538-4357

Publisher:: Institute of Physics (IOP)Copyright Statement

Country of Publication:: United States

Language:: English

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Cited by: 18 works

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79 ASTRONOMY AND ASTROPHYSICS
circumstellar matter
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nuclear reactions
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abundances–stars: AGB and post-AGB–stars: carbon