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  2. Proton–proton chain - Wikipedia

    en.wikipedia.org/wiki/Proton–proton_chain

    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 ...

  3. Nuclear fusion - Wikipedia

    en.wikipedia.org/wiki/Nuclear_fusion

    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 ...

  4. Nucleosynthesis - Wikipedia

    en.wikipedia.org/wiki/Nucleosynthesis

    Synthesis of these elements occurred through nuclear reactions involving the strong and weak interactions among nuclei, and called nuclear fusion (including both rapid and slow multiple neutron capture), and include also nuclear fission and radioactive decays such as beta decay. The stability of atomic nuclei of different sizes and composition ...

  5. Explained: What nuclear fusion breakthrough means [Video] - AOL

    www.aol.com/news/nuclear-fusion-could-change...

    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 ...

  6. The Hope and Hype of Fusion Energy, Explained - AOL

    www.aol.com/news/hope-hype-fusion-energy...

    Advances in the potential energy source may not be about electricity, at least at first.

  7. Neutrinos from our Sun hold the secrets to nuclear fusion

    www.aol.com/neutrinos-sun-hold-secrets-nuclear...

    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.

  8. Silicon-burning process - Wikipedia

    en.wikipedia.org/wiki/Silicon-burning_process

    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.

  9. Stellar nucleosynthesis - Wikipedia

    en.wikipedia.org/wiki/Stellar_nucleosynthesis

    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.