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Nuclear fusion–fission hybrid (hybrid nuclear power) is a proposed means of generating power by use of a combination of nuclear fusion and fission processes. The concept dates to the 1950s, and was briefly advocated by Hans Bethe during the 1970s, but largely remained unexplored until a revival of interest in 2009, due to the delays in the ...
At the Sun's core temperature of 15.5 million K the PP process is dominant. The PP process and the CNO process are equal at around 20 MK. [1] Scheme of the proton–proton branch I reaction. The proton–proton chain, also commonly referred to as the p–p chain, is one of two known sets of nuclear fusion reactions by which stars convert ...
The ejected material will contain the helium and carbon produced by the Sun's nuclear reactions, continuing the enrichment of the interstellar medium with heavy elements for future generations of stars and planets. [129] The Ring nebula, a planetary nebula similar to what the Sun will become
Advances in the potential energy source may not be about electricity, at least at first.
Nuclear fusion seeks to replicate the reaction that makes the sun and other stars shine, by fusing together two atoms to unleash huge amounts of energy. Often referred to as the holy grail of ...
The first of these, the proton-proton (pp) reaction is the simpler, as well as the more common, of the two. Typically, there are two processes by which smaller stars create fusion.
The reaction rate density between species A and B, having number densities n A,B, is given by: = where k is the reaction rate constant of each single elementary binary reaction composing the nuclear fusion process: = here, σ(v) is the cross-section at relative velocity v, and averaging is performed over all velocities.
In astrophysics, silicon burning is a very brief [1] sequence of nuclear fusion reactions that occur in massive stars with a minimum of about 8–11 solar masses. Silicon burning is the final stage of fusion for massive stars that have run out of the fuels that power them for their long lives in the main sequence on the Hertzsprung–Russell diagram.