Black holes are formed when massive stars undergo gravitational collapse at the end of their life cycle.

The minimum mass required for a star to form a black hole is known as the Chandrasekhar limit, which is approximately 1.4 solar masses.

The event horizon is the boundary in spacetime beyond which the gravitational pull becomes so strong that nothing, not even light, can escape.

The singularity at the center of a black hole is a point where the laws of physics, as we currently understand them, break down.

As matter and energy fall into a black hole, they form an accretion disk, which heats up due to friction and releases enormous amounts of radiation.

Spaghettification is the extreme stretching and compression of matter as it approaches a black hole due to the intense gravitational forces.

Hawking radiation is the theoretical emission of particles and energy from black holes due to quantum effects near the event horizon.

A Kerr black hole is a rotating black hole, named after the mathematician Roy Kerr who discovered this solution to Einstein's equations of general relativity.

A Schwarzschild black hole is a non-rotating black hole, named after the mathematician Karl Schwarzschild who discovered this solution to Einstein's equations of general relativity.

M87* is the largest black hole discovered to date, located at the center of the galaxy M87.

V616 Monocerotis is the closest black hole to Earth, located approximately 3,000 light-years away.

Black hole mergers are catastrophic events that occur when two black holes collide and merge into a single larger black hole.

Black hole mergers produce a characteristic gravitational wave signal known as a chirp signal, which increases in frequency as the black holes spiral closer together.

The Event Horizon Telescope is a network of radio telescopes that captured the first direct image of a black hole, located at the center of the galaxy M87.

The first direct image of a black hole provided strong evidence in support of the predictions of Einstein's theory of general relativity.