Carbon-burning process

The carbon-burning process or carbon fusion is a set of nuclear fusion reactions that take place in the cores of massive stars (at least 8 at birth) that combines carbon into other elements. It requires high temperatures (> 5×108 K or 50 keV) and densities (> 3×109 kg/m3). These figures for temperature and density are only a guide. More massive stars burn their nuclear fuel more quickly, since they have to offset greater gravitational forces to stay in (approximate) hydrostatic equilibrium. That generally means higher temperatures, although lower densities, than for less massive stars. To get the right figures for a particular mass, and a particular stage of evolution, it is necessary to use a numerical stellar model computed with computer algorithms. Such models are continually being refined based on nuclear physics experiments (which measure nuclear reaction rates) and astronomical observations (which include direct observation of mass loss, detection of nuclear products from spectrum observations after convection zones develop from the surface to fusion-burning regions – known as dredge-up events – and so bring nuclear products to the surface, and many other observations relevant to models). The principal reactions are: {| border="0" |- style="height:3em;" || ||+ || ||→ || ||+ || ||+ ||4.617 MeV |- style="height:3em;" | ||+ || ||→ || ||+ || ||+ ||2.241 MeV |- style="height:3em;" | ||+ || ||→ || ||+ ||1n ||− ||2.599 MeV |- style="height:3em;" |colspan=99|Alternatively: |- style="height:3em;" | ||+ || ||→ || ||+ ||_Gamma ||+ ||13.933 MeV |- style="height:3em;" | ||+ || ||→ || ||+ ||2 ||colspan=2|− 0.113 MeV |} This sequence of reactions can be understood by thinking of the two interacting carbon nuclei as coming together to form an excited state of the 24Mg nucleus, which then decays in one of the five ways listed above. The first two reactions are strongly exothermic, as indicated by the large positive energies released, and are the most frequent results of the interaction.