Stars function as the universe’s most efficient chemical reactors, driving the synthesis, transformation and redistribution of elements across cosmic time. This review examines the chemical processes underlying stellar birth, evolution and death, with emphasis on molecular, nuclear and isotopic pathways that govern elemental production. We begin with the astrochemistry of star-forming regions, highlighting gas-phase reactions, grain-surface chemistry and molecular complexity in collapsing molecular clouds. The sequential nuclear burning stages hydrogen, helium and advanced burning are discussed in terms of reaction networks, resonance phenomena and reaction-rate sensitivities that control elemental yields. Particular focus is placed on neutron-capture nucleosynthesis (s-, r- and p-processes), detailing their chemical signatures and dominant stellar environments. The chemical feedback from Asymptotic Giant Branch (AGB) stars, Supernovae and Neutron-star mergers is evaluated in the context of isotopic enrichment and elemental recycling into the interstellar medium. Again, unresolved chemical uncertainties, including key reaction rates and heavy-element production pathways are assessed. By integrating astrochemistry, nuclear chemistry and observational constraints, this review presents a coherent chemical framework for understanding the cosmic origin and evolutionary trend of the elements.
Stellar nucleosynthesis; Astrochemistry; Nuclear burning; Neutron-capture processes (s-process, r-process, p-process); Asymptotic Giant Branch (AGB) stars; Supernovae; Neutron star mergers; Interstellar medium; Galactic chemical evolution; Molecular clouds.
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