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Nuclear fusion combines atomic nuclei to create a heavier nucleus.
Nuclear fusion is a nuclear reaction in which two or more atomic nuclei combine to form a larger nucleus. The difference in nuclear binding energy between the reactants and products appears as released or absorbed energy. Fusion of light nuclei, especially hydrogen isotopes such as deuterium and tritium, generally releases energy because the resulting nucleus is more tightly bound. Fusion requires nuclei to overcome their electrostatic repulsion, typically through extremely high temperatures and suitable density and confinement time. It powers stars, where hydrogen nuclei fuse into helium, and is being studied for energy production using approaches such as magnetic confinement in tokamaks and stellarators and inertial confinement with lasers.
Nuclear fusion combines atomic nuclei to create a heavier nucleus.
Fusion of light elements can release substantial energy because of increased nuclear binding energy.
The extreme conditions needed for fusion occur naturally in stars and are recreated in fusion research devices.
Deuterium–tritium fusion is a leading reaction for experimental fusion energy because it produces helium, a neutron, and significant energy.
A nuclear reaction in which two or more atomic nuclei combine to form a larger nucleus.
The energy that holds protons and neutrons together within an atomic nucleus.
A fusion reaction between deuterium and tritium that produces helium-4, a neutron, and about 17.6 MeV of energy.
Fusion driven by extremely high temperatures that give nuclei enough kinetic energy to overcome their electrostatic repulsion.
The electrostatic repulsion that positively charged atomic nuclei must overcome before they can fuse.
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