form helium in the proton–proton chain reaction: 41H → 22H + 2e+ + 2νe(2 x 0.4 MeV) 2e+ + 2e− → 2γ (2 x 1.0 MeV) 21H + 22H → 23He + 2γ (2 x 5.5 MeV) 23He → 4He + 21H (12.9 MeV) There are a couple other paths, in which He and He combine to form Be, which eventually (with the addition of another proton) yields two He, a gain of one. All these reactions result in the overall reaction: 41H → 4He + 2γ + 2νe (26.7 MeV) where γ is a gamma ray photon, νe is a neutrino, and H and He are isotopes of hydrogen and helium, respectively. The energy released by this reaction is in millions of electron volts. Each individual reaction produces only a tiny amount of energy, but because enormous numbers of these reactions occur constantly, they produce all the energy necessary to sustain the star's radiation output. In comparison, the combustion of two hydrogen gas molecules with one oxygen gas molecule releases only 5.7 eV. In more massive stars, helium is produced in a cycle of reactions catalyzed by carbon called the carbon-nitrogen-oxygen cycle. In evolved stars with cores at 100 million kelvin and masses between 0.5 and 10 , helium can be transformed into carbon in the triple-alpha process that uses the intermediate element beryllium: 4He + 4He + 92 keV → 8*Be 4He + 8*Be + 67 keV → 12*C 12*C → 12C + γ + 7.4 MeV For an overall reaction of: 34He → 12C + γ + 7.2 MeV In massive stars, heavier elements can be burned in a contracting core through the neon-burning process and oxygen-burning process. The final stage in the stellar nucleosynthesis process is the silicon-burning process that results in the production of the stable isotope iron-56. Any further fusion would be an endothermic process that consumes energy, and so further energy can only be produced through gravitational collapse. See also Fusor (astronomy) Outline of astronomy Sidereal time Star clocks Star count Stars and planetary systems in fiction References External links Stellar astronomy Concepts in astronomy Light sources