What are the stages in the evolution of a high-mass star?

The stages in the evolution of a high-mass star are protostar, main sequence, red supergiant, supernova, and either a neutron star or black hole.

A high-mass star begins as a protostar, a dense cloud of gas and dust that collapses under its own gravity. As the protostar becomes denser and hotter, nuclear fusion reactions begin in its core, and it enters the main sequence phase. During this phase, the star fuses hydrogen into helium, releasing energy that counteracts the force of gravity.

Once the hydrogen in the core is exhausted, the star expands and cools, becoming a red supergiant. In this phase, the star fuses heavier elements in its core, producing energy and creating heavier elements through nuclear fusion.

Eventually, the star will explode in a supernova, a violent explosion that releases a vast amount of energy and creates heavy elements. The core of the star collapses, either forming a neutron star or a black hole, depending on the mass of the star.

Neutron stars are incredibly dense, with a mass greater than that of the sun but a radius of only a few kilometers. Black holes are even denser, with a gravitational pull so strong that nothing, not even light, can escape their grasp.

The evolution of high-mass stars is important for understanding the formation of heavy elements and the role of supernovae in shaping the universe.