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In general, proton–proton fusion can occur only if the [[kinetic energy]] (i.e. [[temperature]]) of the protons is high enough to overcome their mutual [[Coulomb repulsion|electrostatic repulsion]].<ref>[[Ishfaq Ahmad]], ''The Nucleus'', '''1''': 42, 59, (1971), The Proton type-nuclear fission reaction.</ref>
▲on]]s are the much more common result of proton–proton reactions within the star, and diprotons almost immediately decay back into two protons. Since the conversion of hydrogen to helium is slow, the complete conversion of the hydrogen initially in the [[solar core|core of the Sun]] is calculated to take more than ten billion years.<ref>Kenneth S. Krane, ''Introductory Nuclear Physics'', Wiley, 1987, p. 537.</ref>
Although sometimes called the "proton–proton chain reaction", it is not a [[chain reaction]] in the normal sense. In most nuclear reactions, a chain reaction designates a reaction that produces a product, such as neutrons given off during [[nuclear fission|fission]], that quickly induces another such reaction.
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