The slow neutron capture process (s-process), characterized by the gradual accumulation of neutrons within nuclei, characterizes the quiescent burnings of massive star evolution and the asymptotic giant branch (AGB) phase of low and intermediate mass stars. There, light elements are transformed into heavier ones by means of relatively mild neutron densities (nn$\approx$106-107 cm-3).
In stark contrast, the intermediate neutron capture process (i-process) offers a glimpse into the regime of higher neutron densities (nn$\approx$1015 cm-3), which boost the production of isotopes on the neutron-rich side of the $\beta$ stability valley. As we delve into the still rather unexplored environment of i-process nucleosynthesis, we face the challenges of theoretical modeling and observational validation, striving to unravel the enigmatic genesis of this process.
Lastly, the rapid neutron capture process (r-process) stands as an emblem of cosmic extremity, characterized by incredibly high neutron densities (nn>1023 cm-3). From the powerful supernovae to the exotic landscapes of neutron star mergers, the r-process synthesizes half of the elements heavier than iron, enriching the Universe with the remnants of stellar explosions.
Through meticulous observational studies, theoretical modeling and precise laboratory measurements, we aim at fully understanding the complex details of these neutron capture processes and their profound implications for galactic chemical evolution.
