In the context of stellar evolution, what typically occurs to high-mass stars at the end of their lifespan?

High-mass stars, typically those with a mass greater than approximately eight times that of the Sun, undergo a dramatic end to their lifecycle. After exhausting their nuclear fuel, these stars cannot support themselves against gravitational collapse. The core of a high-mass star collapses under its own gravity, leading to extreme temperatures and pressures.

As a result, the outer layers of the star are expelled violently, resulting in a supernova explosion. This catastrophic event not only disperses elements into space, enriching the interstellar medium but also can leave behind a remnant core. Depending on the mass of the core left after the supernova, this remnant may become a neutron star or, if massive enough, even collapse further into a black hole.

In contrast, other scenarios like becoming white dwarfs, shrinking into neutron stars, or turning into red giants are typical of lower-mass stars or represent different stages of stellar evolution that do not apply to high-mass stars at the end of their lifespan. This highlights the distinct evolutionary paths based on a star’s initial mass.