Silicon-burning process

In astrophysics, silicon burning is a very brief[1] sequence of nuclear fusion reactions that occur in massive stars with a minimum of about 8–11 solar masses.

Silicon burning is the final stage of fusion for massive stars that have run out of the fuels that power them for their long lives in the main sequence on the Hertzsprung–Russell diagram.

Silicon burning begins when gravitational contraction raises the star's core temperature to 2.7–3.5 billion kelvins (GK).

[6] However, since no additional heat energy can be generated via new fusion reactions, the final unopposed contraction rapidly accelerates into a collapse lasting only a few seconds.

[10] The outer layers of the star are blown off in an explosion known as a Type II supernova that lasts days to months.

Conversely, heavy elements such as uranium release energy when broken into lighter elements—the process of nuclear fission.