Alpha-Capture Reaction Rate for $$^{22}$$ Ne( $$\alpha $$ , n) via Sub-Coulomb $$\alpha $$ -Transfer and Its Effect on Final Abundances of s-Process Isotopes

Author(s):  
H. Jayatissa ◽  
G. V. Rogachev ◽  
V. Z. Goldberg ◽  
E. Koshchiy ◽  
B. T. Roeder ◽  
...  
2020 ◽  
Vol 123 ◽  
pp. 102481
Author(s):  
S.B. Dubovichenko ◽  
N.A. Burkova ◽  
A.V. Dzhazairov-Kakhramanov ◽  
A.S. Tkachenko

2016 ◽  
Vol 665 ◽  
pp. 012042 ◽  
Author(s):  
Z Korkulu ◽  
N Özkan ◽  
G G Kiss ◽  
T Szücs ◽  
Zs Fülöp ◽  
...  

2018 ◽  
Author(s):  
A. C. Dreyfuss ◽  
K. D. Launey ◽  
J. E. Escher ◽  
R. B. Baker ◽  
J. P. Draayer ◽  
...  

2014 ◽  
Vol 9 (S307) ◽  
pp. 211-212
Author(s):  
Agnès Bischoff-Kim

AbstractHigh mass and low mass stars follow a similar evolution until the inert core phase that follows the end of the core helium burning stage. In particular, one common phase of stellar evolution is the alpha capture reaction that turns carbon into oxygen in the core. We can obtain constraints on this reaction rate by studying the remnants of low mass stars, as this is the ultimate reaction that occurs in their core. We also present results that allow us to test the time dependent calculations of diffusion in dense interiors.


Author(s):  
S. B. Dubovichenko ◽  
N. A. Burkova ◽  
R. R. Shamitova

2019 ◽  
Vol 49 (1) ◽  
pp. 129-132
Author(s):  
Oliver Forstner ◽  
Daniel Bemmerer ◽  
Thomas E. Cowan ◽  
Rugard Dressler ◽  
Arnd R. Junghans ◽  
...  

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