Oxygen-burning process

Pre-oxygen burning

Although ¹⁶O is lighter than neon, neon burning occurs before oxygen burning, because ¹⁶O is a doubly-magic nucleus and hence extremely stable. Compared to oxygen, neon is much less stable. As a result, neon burning occurs at lower temperatures than ¹⁶O + ¹⁶O. During neon burning, oxygen and magnesium accumulate in the core of the star. At the onset of oxygen burning, oxygen in the stellar core is plentiful due to the helium-burning process (⁴He(2α,γ)¹²C(α,γ)¹⁶O), carbon-burning process (¹²C(¹²C,α)²⁰Ne, ¹²C(α,γ)¹⁶O), and neon-burning process (²⁰Ne(γ,α)¹⁶O). The reaction ¹²C(α,γ)¹⁶O has a significant effect on the reaction rates during oxygen burning, as it produces large quantities of ¹⁶O.

Convectively bounded flames and off-center oxygen ignition

For stars with masses greater than 10.3 solar masses, oxygen ignites in the core or not at all. Similarly, for stars with a mass of less than 9 solar masses (without accretion of additional mass) oxygen ignites in the core or not at all. However, in the 9–10.3 solar mass range, oxygen ignites off-center.

For stars in this mass range neon-burning occurs in a convective envelope rather than at the core of the star. For the particular example of a 9.5 solar mass star, the neon-burning process takes place in an envelope of approximately 0.252 solar masses (~1560 kilometers) off center. From the ignition flash, the neon convective zone extends further out to 1.1 solar masses with a peak power around 10³⁶ W. After only a month, the power declines to about 10³⁵ W and stays at this rate for about 10 years. After this phase, the neon in the shell is depleted, resulting in greater inward pressure on the star. This raises the shell's temperature to 1.65 billion kelvins. This results in a neon-burning, convectively-bound flame front that moves toward the core. The motion of the flame is what eventually leads to oxygen-burning. In approximately 3 years, the flame's temperature reaches about 1.83 billion kelvins, enabling the oxygen-burning process to commence. This occurs around 9.5 years before the iron core develops. Similarly to the beginning of neon-burning, off-center oxygen-burning commences with another flash. The convectively burning flame then results from both neon and oxygen burning as it advances towards the core, while the oxygen-burning shell continuously shrinks in mass.

Neutrino losses

During the oxygen-burning process, energy loss due to neutrino emission becomes relevant. Due to the large energy loss, oxygen must burn at temperatures higher than a billion kelvins in order to maintain a radiation pressure strong enough to support the star against gravity. Further, two electron capture reactions (which produce neutrinos) become significant when the matter density is high enough (ρ > 2×10⁷ g/cm³). Due to these factors, the timescale of oxygen burning is much shorter for heavy, dense stars.

Explosive oxygen burning

The oxygen-burning process can occur under hydrostatic and under explosive conditions. The products of explosive oxygen burning are similar to those in hydrostatic oxygen burning. However, stable oxygen burning is accompanied by a multitude of electron captures, while explosive oxygen burning is accompanied by a significantly greater presence of photodisintegration reactions. In the temperature range of (3–4)×10⁹ K, photodisintegration and oxygen fusion occur with comparable reaction rates.

Pair-instability supernovae

Very massive (140–260 solar masses) population III stars may become unstable during core oxygen burning due to pair production. This results in a thermonuclear explosion, which completely disrupts the star.