The Black Holes

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

As matter approaches the event horizon, it is stretched and compressed by the intense gravitational forces, a phenomenon known as spaghettification.

The singularity is the point at the center of a black hole where all matter is compressed into an infinitely small volume, resulting in infinite density and gravity.

The Schwarzschild radius is the radius of the event horizon of a black hole, which is determined by its mass.

Hawking radiation is the thermal radiation emitted by black holes due to quantum effects near the event horizon.

The Penrose process involves throwing an object into a black hole and then extracting energy from the resulting radiation.

The ergosphere is the region outside the event horizon where objects can orbit the black hole without falling into it.

Black holes and white holes are hypothetical objects with opposite properties. Black holes absorb matter and energy, while white holes expel matter and energy.

The Tolman-Oppenheimer-Volkoff limit is the maximum mass a black hole can have before it collapses under its own gravity.

The mass of a black hole is directly proportional to the radius of its event horizon, as determined by the Schwarzschild radius formula.

Accretion is the process by which matter falls onto a black hole, forming an accretion disk around it.

Cygnus X-1 was the first black hole ever discovered, identified in 1971.

Sagittarius A* is the supermassive black hole at the center of our galaxy, the Milky Way.

M87* is the supermassive black hole at the center of the galaxy M87, which is famous for its iconic image captured by the Event Horizon Telescope.

GRO J1655-40 is the closest known black hole to Earth, located about 10,000 light-years away.