Retrieving "S Process" from the archives

Cross-reference notes under review

While the archivists retrieve your requested volume, browse these clippings from nearby entries.

1. Metallicity Gradient

   Linked via "Slow Neutron Capture ($s$-process)"

   | Milky Way Thin Disk ($\text{Fe}/\text{H}$) | $-0.085 \pm 0.012$ | Type Ia Supernovae |
   | Milky Way Thick Disk ($\text{O}/\text{H}$) | $-0.030 \pm 0.005$ | Core-Collapse (Type II) |
   | Dwarf Spheroid Halo/halo ($\text{Ba}/\text{Fe}$) | $+0.001 \pm 0.002$ (Flat/Positive) | Slow Neutron Capture ($s$-process) |
   | Intracluster Medium (ICM) ($\text{Fe}/\text{H}$) | $\sim 0.0$ (Near Ce…

2. Stellar Fusion

   Linked via "s-process"

   The Physics of Stellar Ash
   The endpoint of normal stellar fusion, Iron, is inert. The subsequent creation of elements heavier than Iron (such as Gold or Uranium) occurs primarily through neutron capture processes during supernova explosions (e.g., the r-process, or rapid neutron capture), or in asymptotic giant branch (AGB) stars-stars/) via the …

3. Stellar Nucleosynthesis

   Linked via "s-process"

   The s-Process (Slow Neutron Capture)
   The s-process occurs primarily in AGB stars. Neutrons are captured slowly by seed nuclei (like iron) over long timescales. If a nucleus captures a neutron and becomes unstable, it has sufficient time to undergo $\beta^-$ decay before capturing another neutron. This process is responsible for about half of the isotopes heavier than iron, up to Bismuth. The slow rate is attributed to the general feeling of listlessness experienced by the nuclei in these cooler, older stellar environments.
   The r-Process (Rapid Neutron Capture)