Low-Mass Stars (like our Sun):
* White Dwarf: After shedding its outer layers as a planetary nebula, the core of a low-mass star collapses into a dense, hot, and very small white dwarf. This is primarily composed of carbon and oxygen. White dwarfs slowly cool over billions of years.
Medium-Mass Stars (slightly more massive than the Sun):
* Neutron Star: These stars have enough gravity to overcome electron degeneracy pressure, causing protons and electrons to combine to form neutrons. This creates a incredibly dense object with a radius of only a few kilometers. Neutron stars are incredibly hot and emit powerful radio waves, sometimes leading to the formation of pulsars.
High-Mass Stars (significantly more massive than the Sun):
* Black Hole: When a massive star collapses, the gravity is so intense that even the neutron degeneracy pressure cannot withstand it. The core collapses into a singularity, a point of infinite density, surrounded by an event horizon - a region of spacetime where gravity is so strong that nothing, not even light, can escape.
Key Points:
* Stellar Evolution: The collapse of a star's core is a natural process in stellar evolution.
* Elements: During the star's lifetime, fusion creates heavier elements, eventually reaching iron, which is very stable and cannot be fused further.
* Supernovae: The collapse of a massive star can trigger a supernova explosion, scattering heavy elements into space, enriching the universe.
It's worth noting that the exact endpoint of a star's life is a complex process influenced by factors like its initial mass, rotation, and the presence of a companion star.
