The Three Dimensional Evolution to Core Collapse of a Massive Star

Understand

We present the first three dimensional (3D) simulation of the final minutes of iron core growth in a massive star, up to and including the point of core gravitational instability and collapse.

• We self-consistently capture the development of strong convection driven by violent Si burning in the shell surrounding the iron core.
• This convective burning builds the iron core to its critical (Chandrasekhar) mass and collapse ensues, driven by electron capture and photodisintegration.
• The non-spherical structure and motion (turbulent fluctuations) generated by 3D convection is substantial at the point of collapse.