How a star's mass decides its end: white dwarfs, neutron stars, and black holes

A star's mass on the main sequence decides how it will end. A low- or medium-mass star like the Sun swells into a red giant, gently sheds its outer layers as a glowing planetary nebula, and leaves behind its hot core as a white dwarf, an object about the size of Earth but so dense that a teaspoon of it would weigh tons on Earth. A star born with more than about 8 times the Sun's mass fuses heavier and heavier elements until it builds an iron core, which collapses and triggers a supernova explosion. What remains of the core becomes a neutron star, only about 20 kilometers across yet more massive than the Sun, packed as densely as an atomic nucleus; rapidly spinning neutron stars can appear as pulsars. If the leftover core is too massive, more than roughly 2 to 3 times the Sun's mass, nothing can stop its collapse, and it becomes a black hole, whose gravity is so strong that not even light can escape from inside its event horizon.

This explanation is AI-generated and can occasionally be wrong.

Vibistic AI

🔒 We never store your messages. The free built-in AI runs through Vibistic's own server, on Cloudflare's own AI infrastructure. You can also add your own API key to send messages straight from your browser to your AI provider instead.

Ask a question about How a star's mass decides its end: white dwarfs, neutron stars, and black holes, like "can you give me another example?"