Heavy, less stable nuclei like Uranium-235 split into smaller fragments. These fragments are closer to the iron peak, meaning they have higher binding energy and release the "missing" energy during the split. Stellar Nucleosynthesis
The shape of the curve dictates how we can extract energy from the atom:
Light nuclei move "up" the curve to become more stable by fusing together. This process powers stars like our Sun. The curve of binding energy
. Nuclei in this "iron peak" (notably and Nickel-62 ) are the most tightly bound and stable in the universe.
) . It illustrates the stability of atomic nuclei and explains why certain nuclear reactions—like fusion and fission—release energy. Peak Stability: The curve peaks around a mass number of to Heavy, less stable nuclei like Uranium-235 split into
The curve of binding energy is a graph that plots against the atomic mass number (
), indicating that nuclear forces are "saturated" in mid-sized nuclei. This process powers stars like our Sun
For very light elements like Hydrogen, the binding energy is low but increases sharply as mass number increases. This steep gradient explains why nuclear fusion (combining light nuclei) releases a massive amount of energy.