Nucleosynthesis

Nucleosynthesis

Iron is created in extremely large, extremely hot (over 2.5 billion kelvin) stars, in a process called the silicon burning process. It is the last element to be produced in this manner. The process starts with the second largest stable nucleus created by silicon burning: calcium. One stable nucleus of calcium fuses with one helium nucleus, creating unstable titanium. Before the titanium decays, it can fuse with another helium nucleus, creating unstable chromium. Before the chromium decays, it can fuse with another helium nucleus, creating unstable iron. Before the iron decays, it can fuse with another helium nucleus, creating unstable nickel. The nickel then decays to unstable cobalt, which finally decays to stable iron-56. The iron can no longer be fused with other elements. As the star's core fills with iron, it begins to cool until there is no longer enough energy to maintain its size. It then collapses and the result is a supernova. Supernovas also create additional forms of stable iron via the r-process.









Sacramento Airport
breitling bentley replica