In nuclear fusion, two heavy atoms can merge to form a single, heavier atom by overcoming the electrostatic repulsion between their positively charged nuclei and allowing the strong nuclear force to come into play.
Nuclear fusion involves the combination of atomic nuclei to form a new nucleus. It typically occurs at extremely high temperatures and pressures, such as those found in the core of stars or during controlled fusion reactions in experimental reactors.
The fusion process begins with two atomic nuclei approaching each other closely enough for the strong nuclear force to come into play. The strong nuclear force is the attractive force that binds protons and neutrons within an atomic nucleus. This force is short-range and acts to overcome the electrostatic repulsion between protons due to their positive charges.
When the two nuclei approach each other, if they have enough kinetic energy to overcome the repulsive electrostatic forces, the strong nuclear force can take over. At extremely close distances, the strong nuclear force becomes dominant and attracts the protons and neutrons of the two nuclei together.
As the protons and neutrons from the two nuclei come closer, they may rearrange and combine to form a new nucleus. This process releases a significant amount of energy in the form of light and heat. The resulting nucleus is typically larger and heavier than the original nuclei, as some mass is converted into energy according to Einstein's famous equation, E=mc².
It's important to note that nuclear fusion reactions are highly dependent on specific conditions such as temperature, pressure, and the isotopes involved. Achieving controlled fusion reactions on Earth is a significant scientific and engineering challenge, as it requires creating and sustaining the extreme conditions necessary for fusion to occur.
In nature, nuclear fusion plays a crucial role in powering stars, including our Sun, where hydrogen nuclei combine to form helium through a series of fusion reactions. The release of energy from these reactions sustains the high temperatures and pressures required to maintain stellar equilibrium.