Speaker
Description
By definition, the proton-rich isotopes that cannot be reached by neutron-capture processes are the p-only isotopes or the p-nuclei. However, several p-nuclei can produced by the s process in low-mass AGB stars, e.g. (1) $\mathrm{^{94}Mo}$ by two consecutive neutron captures of $\mathrm{^{92}Mo}$ and following the decay of $\mathrm{^{93}Zr}$ and $\mathrm{^{94}Nb}$, (2) $\mathrm{^{108}Cd}$ depending on the $\mathrm{\beta}$-decay rate of $\mathrm{^{107}Pd}$ and $\mathrm{^{108}Ag}$, and (3) $\mathrm{^{152}Gd}$ due to the operation of $\mathrm{^{151}Sm}$ and $\mathrm{^{152}Eu}$ branching points. We present how the use of temperature- and density-dependent $\mathrm{\beta}$-decay and electron-capture rates instead of terrestrial/constant values affects the production of $\mathrm{^{94}Mo}$, $\mathrm{^{108}Cd}$ and $\mathrm{^{152}Gd}$ in Monash s-process nucleosynthesis models.
| Length of presentation requested | Oral presentation: 8 min + 2 min questions (Poster-type talk) |
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| Please select a keyword related to your abstract | Stellar Models and Galactic Chemical Evolution |
