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Nuclear fusion is the process that powers active or main-sequence stars and other high-magnitude stars, where large amounts of energy are released. A nuclear fusion process that produces atomic nuclei lighter than iron-56 or nickel-62 will generally release energy.
To do this, it must release the absorbed energy. This can happen in various ways. The extra energy can be converted into molecular motion and lost as heat, or re-emitted by the electron as light (fluorescence). The energy, but not the electron itself, may be passed onto another molecule; this is called resonance energy transfer.
The total energy yield of one whole chain is 26.73 MeV. Energy released as gamma rays will interact with electrons and protons and heat the interior of the Sun. Also kinetic energy of fusion products (e.g. of the two protons and the 4 2 He from the p–p I reaction) adds energy to the plasma in the Sun.
Advances in the potential energy source may not be about electricity, at least at first.
Reaction centers are present in all green plants, algae, and many bacteria.A variety in light-harvesting complexes exist across the photosynthetic species. Green plants and algae have two different types of reaction centers that are part of larger supercomplexes known as P700 in Photosystem I and P680 in Photosystem II.
Nuclear fusion is when two light atomic nuclei combine to form a single heavier one and release massive amounts of energy. It’s essentially the more powerful inverse of nuclear fission, a ...
The carbon-burning process or carbon fusion is a set of nuclear fusion reactions that take place in the cores of massive stars (at least 4 at birth) that combines carbon into other elements. It requires high temperatures (> 5×10 8 K or 50 keV) and densities (> 3×10 9 kg/m 3). [1]
The Sun, like other stars, is a natural fusion reactor, where stellar nucleosynthesis transforms lighter elements into heavier elements with the release of energy. Binding energy for different atomic nuclei.