The Imprint of Nova Nucleosynthesis in Presolar Grains

2002 ◽  
Author(s):  
Jordi José
Keyword(s):  
Presolar Grains

scholarly journals Sputtering of Presolar Grains via Galactic Cosmic Rays in the Interstellar Medium

2020 ◽  
Vol 905 (1) ◽  
pp. 80
Author(s):  
Akshat Garg ◽  
Kuljeet K. Marhas ◽  
Vikram Goyal
Keyword(s):  
Cosmic Rays ◽  
Interstellar Medium ◽  
Galactic Cosmic Rays ◽  
Presolar Grains

scholarly journals Presolar grains

2010 ◽  
Author(s):  
Andrew Davis ◽  
Roberto Gallino
Keyword(s):  
Presolar Grains

scholarly journals CARBON-RICH PRESOLAR GRAINS FROM MASSIVE STARS: SUBSOLAR 12 C/ 13 C AND 14 N/ 15 N RATIOS AND THE MYSTERY OF 15 N

2015 ◽  
Vol 808 (2) ◽  
pp. L43 ◽  
Author(s):  
M. Pignatari ◽  
E. Zinner ◽  
P. Hoppe ◽  
C. J. Jordan ◽  
B. K. Gibson ◽  
...  
Keyword(s):  
Massive Stars ◽  
Presolar Grains

scholarly journals On the Mass and Metallicity Distributions of the Parent AGB Stars of O-Rich Presolar Stardust Grains

2009 ◽  
Vol 26 (3) ◽  
pp. 271-277 ◽  
Author(s):  
Larry R. Nittler
Keyword(s):  
Molecular Clouds ◽  
Asymptotic Giant Branch ◽  
Agb Stars ◽  
Isotopic Data ◽  
Intermediate Mass ◽  
Presolar Grains ◽  
Model Predictions ◽  
The Galaxy ◽  
Low Metallicity ◽  
The Masses

AbstractPresolar grains in meteorites formed in a sample of Asymptotic Giant Branch (AGB) stars that ended their lives within ≈1 Gyr of the origin of the Solar System 4.6 Gyr ago. The O-isotopic compositions of presolar O-rich stardust reflect the masses and metallicities of their parent stars. We present simple Monte Carlo simulations of the parent AGB stars of presolar grains. Comparison of model predictions with the grain data allow some broad conclusions to be drawn: (1) Presolar O-rich grains formed in AGB stars of mass ∼1.15–2.2 M⊙. The upper-mass cutoff reflects dredge-up of C in more massive AGB stars, leading to C-rich dust rather than O-rich, but the lack of grains from intermediate-mass AGB stars (>4 M⊙) is a major puzzle; (2) The grain O-isotopic data are reproduced well if the Galaxy in presolar times was assumed to have a moderate age-metallicity relationship, but with significant metallicity scatter for stars born at the same time; (3) The Sun appears to have a moderately low metallicity for its age and/or unusual 17O/16O and 18O/16O ratios for its metallicity; and (4) The Solar 17O/18O ratio, while unusual relative to present-day molecular clouds and protostars, was not atypical for the presolar disk and does not require self-pollution of the protosolar molecular cloud by supernova ejecta.

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