🌌 SIMULATION OF A BLACK HOLE
Observe events on the horizon, accretion disk, and spacetime curvature.
🔬 Black Hole Structure
SINGULARITY
The center of a black hole, where gravity becomes infinite. Here, the laws of physics cease to function, and space and time lose their meaning. The singularity has zero volume and infinite density.
Event horizon
The boundary around a black hole beyond which nothing, not even light, can escape the gravitational pull. This is the point of no return - anything that crosses the event horizon disappears forever from an outside observer.
Accretion disk
The substance is orbiting a black hole that is pulling it in. As it approaches the event horizon, the substance heats up to millions of degrees, emitting X-rays and light.
Relativistic jets
High plasma jets escaping the poles of a black hole at speeds close to the speed of light. They form due to interaction between the magnetic field and the accretion disk.
⚡ Types of Black Holes
Stellar black holes
Formed after the collapse of massive stars (more than 20 solar masses). Mass from 3 to 100 solar masses. Located in stellar systems and globular clusters.
Supermassive black holes
Located in galactic centers, including the Milky Way. Masses from millions to billions of solar masses. Influence galaxy and stellar system evolution.
Intermediate black holes
Mass from 100 to 100,000 solar masses. Can form through the merger of stellar black holes or as a result of the collapse of extremely massive stars.
Primordial black holes
Hypothetical black holes that could have formed in early Universe due to density fluctuations. They may have masses ranging from microscopic to stellar sizes.
❓ Frequently Asked Questions
As you approach the event horizon, you will experience the "spaghettification" effect — gravitational forces will stretch your body. Beyond the event horizon, you can never return, and singularity will tear you apart at the atomic level.
Theoretical radiation that arises near the event horizon due to quantum fluctuations in vacuum. A black hole slowly "evaporates", losing mass. For large black holes, this process takes trillions of years.
It is impossible to see a black hole directly, but its effects can be observed: accretion disk, relativistic jets, bending of light from stars behind it. In 2019, the first image of a black hole's shadow was obtained.
White holes are theoretical objects opposite to black holes. They could emit matter and light but not absorb them. Physicists consider them unlikely in the real Universe.
The nearest known black hole is V616 Monocerotis (A0620-00) at a distance of 3,000 light years. A supermassive black hole Sagittarius A* is located in the center of our galaxy at a distance of 26,000 light years.