Oxygen-burning process | Wikipedia audio article | Wikipedia audio article
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Date: 18/11/2018

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Oxygen-burning process | Wikipedia audio article

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- Socrates



SUMMARY
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The oxygen-burning process is a set of nuclear fusion reactions that take place in massive stars that have used up the lighter elements in their cores. Oxygen-burning is preceded by the neon-burning process and succeeded by the silicon-burning process. As the neon-burning process ends, the core of the star contracts and heats until it reaches the ignition temperature for oxygen burning. Oxygen burning reactions are similar to those of carbon burning; however, they must occur at higher temperatures and densities due to the larger Coulomb barrier of oxygen. Oxygen in the core ignites in the temperature range of (1.5-2.6)×109 K and in the density range of (2.6-6.7)×109g/cm3. The principal reactions are given below, where the branching ratios assume that the deuteron channel is open (at high temperatures):

Near 2×109K, the oxygen burning reaction rate is approximately 2.8×10−12(T9/2)33, where T9 is the temperature in billions of Kelvin. Overall, the major products of the oxygen-burning process are  28Si, 32,33,34S, 35,37Cl, 36,38Ar, 39,41K,  and 40,42Ca. Of these, 28Si and 32S constitute 90% of the final composition. The oxygen fuel within the core of the star is exhausted after 0.01–5 years depending on the star’s mass and other parameters. The silicon-burning process which follows creates iron, but this iron cannot react further to create energy to support the star. 
During the oxygen-burning process, proceeding outward, there is an oxygen-burning shell, followed by a neon shell, a carbon shell, a helium shell, and a hydrogen shell. The oxygen-burning process is the last nuclear reaction in the star's core which does not proceed via the alpha process.