scholarly journals Do meteoritic silicon carbide grains originate from asymptotic giant branch stars of super-solar metallicity?

2018 ◽  
Vol 221 ◽  
pp. 6-20 ◽  
Author(s):  
Maria Lugaro ◽  
Amanda I. Karakas ◽  
Mária Pető ◽  
Emese Plachy
Keyword(s):  
Silicon Carbide ◽  
Asymptotic Giant Branch ◽  
Asymptotic Giant Branch Stars ◽  
Solar Metallicity ◽  
Giant Branch Stars

Finite Temperature Behavior of Carbon Atom Doped Silicon Clusters: Depressed Thermal Stabilities, Co-existing isomers, Reversible Dynamical Pathways and Fragmentation Channels

2021 ◽  
Author(s):  
Krati Joshi ◽  
Ashakiran Maibam ◽  
Sailaja Krishnamurty
Keyword(s):  
Silicon Carbide ◽  
Carbon Atom ◽  
Finite Temperature ◽  
Asymptotic Giant Branch ◽  
Temperature Behavior ◽  
Asymptotic Giant Branch Stars ◽  
Silicon Clusters ◽  
Thermal Stabilities ◽  
Doped Silicon ◽  
Giant Branch Stars

Silicon carbide clusters are significant due to their predominant occurrence in meteoric star dust, particularly in carbon rich asymptotic giant branch stars. Of late, they have also been recognized as...

scholarly journals Stellar Models and Yields of Asymptotic Giant Branch Stars

2007 ◽  
Vol 24 (3) ◽  
pp. 103-117 ◽  
Author(s):  
Amanda Karakas ◽  
John C. Lattanzio
Keyword(s):  
Main Sequence ◽  
Asymptotic Giant Branch ◽  
Asymptotic Giant Branch Stars ◽  
Agb Stars ◽  
Population Synthesis ◽  
Intermediate Phases ◽  
Structural Details ◽  
Solar Metallicity ◽  
Stellar Models ◽  
Giant Branch Stars

AbstractWe present stellar yields calculated from detailed models of low and intermediate-mass asymptotic giant branch (AGB) stars. We evolve models with a range of mass from 1 to 6 M⊙, and initial metallicities from solar to 1/200th of the solar metallicity. Each model was evolved from the zero age main sequence to near the end of the thermally pulsing (TP) AGB phase, and through all intermediate phases including the core He-flash for stars initially less massive than 2.5 M⊙. For each mass and metallicity, we provide tables containing structural details of the stellar models during the TP-AGB phase, and tables of the stellar yields for 74 species from hydrogen through to sulfur, and for a small number of iron-group nuclei. All tables are available for download. Our results have many applications including use in population synthesis studies and the chemical evolution of galaxies and stellar systems, and for comparison to the composition of AGB and post-AGB stars and planetary nebulae.

scholarly journals Lifetimes of interstellar dust from cosmic ray exposure ages of presolar silicon carbide

2020 ◽  
Vol 117 (4) ◽  
pp. 1884-1889 ◽  
Author(s):  
Philipp R. Heck ◽  
Jennika Greer ◽  
Levke Kööp ◽  
Reto Trappitsch ◽  
Frank Gyngard ◽  
...  
Keyword(s):  
Silicon Carbide ◽  
Interstellar Medium ◽  
Interstellar Dust ◽  
Particle Flux ◽  
Cosmic Ray ◽  
Asymptotic Giant Branch ◽  
Asymptotic Giant Branch Stars ◽  
Exposure Ages ◽  
Giant Branch Stars ◽  
Cosmic Ray Exposure Ages

We determined interstellar cosmic ray exposure ages of 40 large presolar silicon carbide grains extracted from the Murchison CM2 meteorite. Our ages, based on cosmogenic Ne-21, range from 3.9 ± 1.6 Ma to ∼3 ± 2 Ga before the start of the Solar System ∼4.6 Ga ago. A majority of the grains have interstellar lifetimes of <300 Ma, which is shorter than theoretical estimates for large grains. These grains condensed in outflows of asymptotic giant branch stars <4.9 Ga ago that possibly formed during an episode of enhanced star formation ∼7 Ga ago. A minority of the grains have ages >1 Ga. Longer lifetimes are expected for large grains. We determined that at least 12 of the analyzed grains were parts of aggregates in the interstellar medium: The large difference in nuclear recoil loss of cosmic ray spallation products 3He and 21Ne enabled us to estimate that the irradiated objects in the interstellar medium were up to 30 times larger than the analyzed grains. Furthermore, we estimate that the majority of the grains acquired the bulk of their cosmogenic nuclides in the interstellar medium and not by exposure to an enhanced particle flux of the early active sun.

scholarly journals Asymptotic giant branch and super-asymptotic giant branch stars: modelling dust production at solar metallicity

2017 ◽  
Vol 467 (4) ◽  
pp. 4431-4440 ◽  
Author(s):  
F. Dell'Agli ◽  
D. A. García-Hernández ◽  
R. Schneider ◽  
P. Ventura ◽  
F. La Franca ◽  
...  
Keyword(s):  
Asymptotic Giant Branch ◽  
Asymptotic Giant Branch Stars ◽  
Dust Production ◽  
Solar Metallicity ◽  
Giant Branch Stars
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