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'''Nuclear fusion''' is the process by which two or more nuclei fuse to make a larger nucleus.<ref>Wile, Dr. Jay L. ''Exploring Creation With Physical Science''. Apologia Educational Ministries, Inc. 1999, 2000</ref> The successful fusion of two light (lighter than iron) nuclei releases large amounts of [[energy]], but to start the reactions large amounts of energy must be input to overcome the repulsive electrostatic forces. The energy is released from the mass in accordance with [[e=mc^2]]. To conserve energy, the mass of the products is less than the reactants.
'''Nuclear fusion''' is the process by which two or more nuclei fuse to make a larger nucleus.<ref>Wile, Dr. Jay L. ''Exploring Creation With Physical Science''. Apologia Educational Ministries, Inc. 1999, 2000</ref> The successful fusion of two light (lighter than iron) nuclei releases large amounts of [[energy]], but to start the reactions large amounts of energy must be input to overcome the repulsive electrostatic forces. The energy is released from the mass in accordance with [[e=mc^2|E=mc<sup>2</sup>]]. To conserve energy, the mass of the products is less than the reactants.
In the center of most stars, hydrogen fuses together to form helium. Fusion in stars releases so much heat that the process alone keeps their mass from collapsing in on itself due to [[gravity]]. It is the reason that stars are so stable as well. If the core of a star starts to collapse, more fusion reactions occur and it expands again from the heat. If the core expands too far, less fusion reactions occur and it collapses back down. This can repeat until iron 56 is reached, at which point it becomes energetically unfavorable to continue. It requires [[energy]] to advance further rather than energy being released.
In the center of most stars, hydrogen fuses together to form helium. Fusion in stars releases so much heat that the process alone keeps their mass from collapsing in on itself due to [[gravity]]. It is the reason that stars are so stable as well. If the core of a star starts to collapse, more fusion reactions occur and it expands again from the heat. If the core expands too far, less fusion reactions occur and it collapses back down. This can repeat until iron 56 is reached, at which point it becomes energetically unfavorable to continue. It requires [[energy]] to advance further rather than energy being released.