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  2. Stellar nucleosynthesis - Wikipedia

    en.wikipedia.org/wiki/Stellar_nucleosynthesis

    In astrophysics, stellar nucleosynthesis is the creation of chemical elements by nuclear fusion reactions within stars. Stellar nucleosynthesis has occurred since the original creation of hydrogen, helium and lithium during the Big Bang. As a predictive theory, it yields accurate estimates of the observed abundances of the elements.

  3. Nucleosynthesis - Wikipedia

    en.wikipedia.org/wiki/Nucleosynthesis

    The products of stellar nucleosynthesis are generally dispersed into the interstellar gas through mass loss episodes and the stellar winds of low mass stars. The mass loss events can be witnessed today in the planetary nebulae phase of low-mass star evolution, and the explosive ending of stars, called supernovae , of those with more than eight ...

  4. s-process - Wikipedia

    en.wikipedia.org/wiki/S-process

    The s-process is believed to occur mostly in asymptotic giant branch stars, seeded by iron nuclei left by a supernova during a previous generation of stars. In contrast to the r-process which is believed to occur over time scales of seconds in explosive environments, the s-process is believed to occur over time scales of thousands of years, passing decades between neutron captures.

  5. Oddo–Harkins rule - Wikipedia

    en.wikipedia.org/wiki/Oddo–Harkins_rule

    The Oddo–Harkins rule for elements from 12 C to 56 Fe is explained by the alpha process of stellar nucleosynthesis. [6]: 42 The process involves the fusion of alpha particles (helium-4 nuclei) under high temperature and pressure within the stellar environment. Each step in the alpha process adds two protons (and two neutrons), favoring ...

  6. B2FH paper - Wikipedia

    en.wikipedia.org/wiki/B2FH_paper

    The B 2 FH paper was ostensibly a review article summarising recent advances in the theory of stellar nucleosynthesis. [8] However, it went beyond simply reviewing Hoyle's work, by incorporating observational measurements of elemental abundances published by the Burbidges, and Fowler's laboratory experiments on nuclear reactions.

  7. Triple-alpha process - Wikipedia

    en.wikipedia.org/wiki/Triple-alpha_process

    Fusing with additional helium nuclei can create heavier elements in a chain of stellar nucleosynthesis known as the alpha process, but these reactions are only significant at higher temperatures and pressures than in cores undergoing the triple-alpha process.

  8. Proton–proton chain - Wikipedia

    en.wikipedia.org/wiki/Proton–proton_chain

    This was part of the body of work in stellar nucleosynthesis for which Bethe won the Nobel Prize in Physics in 1967. The proton–proton chain

  9. Alpher–Bethe–Gamow paper - Wikipedia

    en.wikipedia.org/wiki/Alpher–Bethe–Gamow_paper

    Today, nucleosynthesis is widely considered to have taken place in two stages: formation of hydrogen and helium according to the Alpher–Bethe–Gamow theory, and stellar nucleosynthesis of higher elements according to Bethe and Hoyle's later theories.