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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 ...
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 ...
“Fusion, on the other hand, does not create any long-lived radioactive nuclear waste.” The waste byproduct of a fusion reaction is far less radioactive than in fission, and decays far more ...
The CNO cycle (for carbon–nitrogen–oxygen; sometimes called Bethe–Weizsäcker cycle after Hans Albrecht Bethe and Carl Friedrich von Weizsäcker) is one of the two known sets of fusion reactions by which stars convert hydrogen to helium, the other being the proton–proton chain reaction (p–p cycle), which is more efficient at the Sun's ...
Over the last 70 years, there have been several failed attempts to recreate and control the ongoing nuclear fusion reactions that power the sun. Several projects that seemed promising had to be ...
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.
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.
A nuclear fusion reaction, which is what keeps the sun and other stars burning, occurs when the nuclei of two atoms fuse into one atomic nucleus. When that happens, the excess mass converts into ...