Types of Black Holes

Stellar black holes are formed when massive stars exhaust their nuclear fuel and undergo a supernova explosion, leaving behind a collapsed core.

Supermassive black holes are extremely massive black holes, typically millions to billions of times the mass of the Sun, and reside at the centers of galaxies.

Intermediate-mass black holes fall between the mass ranges of stellar and supermassive black holes, typically ranging from 100 to 1000 solar masses.

Primordial black holes are theorized to have formed in the early universe due to density fluctuations during the Big Bang.

Direct collapse black holes are formed when massive gas clouds collapse under their own gravity, bypassing the supernova stage.

The Schwarzschild radius is the radius of the event horizon, the boundary beyond which nothing, not even light, can escape from a black hole.

The ergosphere is the region outside the event horizon where objects can be dragged along by the black hole's rotation, causing them to experience negative energy.

Accretion is the process by which matter, such as gas and dust, falls onto a black hole, releasing energy and increasing its mass.

Hawking radiation is the theoretical emission of particles and radiation from the vicinity of a black hole's event horizon, due to quantum effects.

Spaghettification is the extreme stretching and compression of objects as they approach a black hole's singularity, due to the immense gravitational forces.

Active galactic nuclei (AGN) are supermassive black holes that are actively accreting matter, resulting in the emission of powerful jets and radiation.

Binary black holes are formed when two black holes orbit around each other and eventually merge due to gravitational wave emission.

A singularity is the point of infinite density and gravity at the center of a black hole, where the laws of physics as we know them break down.

Stellar black holes are formed when massive stars collapse under their own gravity after exhausting their nuclear fuel.