From this primordial dominance of hydrogen and helium, newly produced nuclei ejected from nucleosynthesis in stars and explosions gradually built up the cosmic variety of nuclear species currently observed, from carbon to silicon and iron to lead, platinum and uranium (see Fig. 3, Fig. 4. Identify and understand the, Production of heavy elements is one of the main byproducts of the explosive end of massive stars A long-sought goal is to find differentiated patterns in nucleosynthesis yields, which could help identify a number of properties of the explosive core. Among them, traces of the magnetic field topology are particularly abstract. Elements heavier than helium are produced during the life and death of stars. This review explains when and how the process of nucleosynthesis created elements. High-mass stars fuse elements much more quickly, fusing nuclei. heavier and die more catastrophically than low-mass stars. Explosions of high mass stars in the form of supernovae. Four decades ago, the fundamental idea that virtually all elements were made by thermonuclear combustion in the stellar nucleosynthesis of stars was codified 1, 2. Later, astronomical observations 3, 4 suggested that the elements were formed by another process early in cosmological history, perhaps during the Big Bang, nucleosynthesis generally requires physical conditions of high temperatures and densities. They are found in the Big Bang, inside stars and in explosions with their compression shocks and their high fluxes of neutrinos and neutrons. Towards the nucleosynthesis of iron groups, the equilibrium conditions should be strongly favorable. Stellar nitrogen nucleosynthesis. In summary, once a star enters the helium fusion stage, it uses the Triple-alpha process to create carbon from helium, and then uses the Alpha Ladder process to create carbon. oxygen from carbon. Nitrogen, between carbon and oxygen, is produced by decays and is relatively rare compared to Umeda, H. amp Nomoto, K. Nucleosynthesis of zinc and iron Peak Elements in Population III Type II Supernovae. Astrophysics. J. 565, 385-404 2002Stellar nucleosynthesis does not stop at helium. The sequence continues with combinations of nuclei that form the heaviest elements on the periodic table. For example, astronomers have identified more chemical elements in our Sun. oxygen, 0. carbon, 0. iron, 0. nitrogen and, This chapter discusses three nucleosynthesis processes involved in the production of heavy nuclei beyond the iron group that are influenced or shaped by neutrino interactions: the process ν, the νp process and the r process. These processes are all linked to explosive events involving compact objects, such as core collapse,