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  2. Proton–proton chain - Wikipedia

    en.wikipedia.org/wiki/Proton–proton_chain

    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 hydrogen to helium. It dominates in stars with masses less than or equal to that of the Sun , [ 2 ] whereas the CNO cycle , the other known reaction, is suggested by theoretical models to dominate ...

  3. Stellar nucleosynthesis - Wikipedia

    en.wikipedia.org/wiki/Stellar_nucleosynthesis

    Hydrogen fusion (nuclear fusion of four protons to form a helium-4 nucleus [20]) is the dominant process that generates energy in the cores of main-sequence stars. It is also called "hydrogen burning", which should not be confused with the chemical combustion of hydrogen in an oxidizing atmosphere.

  4. Nuclear fusion - Wikipedia

    en.wikipedia.org/wiki/Nuclear_fusion

    The Sun is a main-sequence star, and, as such, generates its energy by nuclear fusion of hydrogen nuclei into helium. In its core, the Sun fuses 620 million metric tons of hydrogen and makes 616 million metric tons of helium each second. The fusion of lighter elements in stars releases energy and the mass that always accompanies it.

  5. Nucleosynthesis - Wikipedia

    en.wikipedia.org/wiki/Nucleosynthesis

    Such a graph of the abundances is displayed on a logarithmic scale below, where the dramatically jagged structure is visually suppressed by the many powers of ten spanned in the vertical scale of this graph. Abundances of the chemical elements in the Solar System. Hydrogen and helium are most common, residuals within the paradigm of the Big ...

  6. B2FH paper - Wikipedia

    en.wikipedia.org/wiki/B2FH_paper

    Arthur Eddington had speculated that the conversion of hydrogen into helium by nuclear fusion could provide the energy required to power stars in 1920. [2] [3] Hans Bethe and Charles L. Critchfield had shown the mechanism for stellar fusion of helium by deriving the proton-proton chain (pp-chain) in 1938. [4]

  7. Supernova nucleosynthesis - Wikipedia

    en.wikipedia.org/wiki/Supernova_nucleosynthesis

    Supernova nucleosynthesis is the nucleosynthesis of chemical elements in supernova explosions.. In sufficiently massive stars, the nucleosynthesis by fusion of lighter elements into heavier ones occurs during sequential hydrostatic burning processes called helium burning, carbon burning, oxygen burning, and silicon burning, in which the byproducts of one nuclear fuel become, after ...

  8. Molecular model - Wikipedia

    en.wikipedia.org/wiki/Molecular_model

    The term, "molecular model" refer to systems that contain one or more explicit atoms (although solvent atoms may be represented implicitly) and where nuclear structure is neglected. The electronic structure is often also omitted unless it is necessary in illustrating the function of the molecule being modeled.

  9. Big Bang nucleosynthesis - Wikipedia

    en.wikipedia.org/wiki/Big_Bang_nucleosynthesis

    In this field, for historical reasons it is customary to quote the helium-4 fraction by mass, symbol Y, so that 25% helium-4 means that helium-4 atoms account for 25% of the mass, but less than 8% of the nuclei would be helium-4 nuclei. Other (trace) nuclei are usually expressed as number ratios to hydrogen.