Created By : awnish

Reviewed By : Rajashekhar Valipishetty

Last Updated : May 23, 2023

Black Hole Collision Calculator helps to know what happens when a black hole collides with another object in the universe. You have to give the before collision parameters such as the black hole mass, event horizon radius before the collision, impacting object details and press the calculate button to get the after collision parameters as result in a blink of an eye.

### What is a Black Hole?

A black hole is a region of spacetime that have strong gravitational acceleration means no particle even light can escape from it. The theory of general relativity can state that a sufficiently compact mass can deform a spacetime to form a black hole. The boundary of the region from which no escape is possible is called the event horizon.

In simple terms, black holes are the objects to work within the universe. The four types of black holes are Stellar black holes, intermediate black holes, supermassive black holes and miniature black holes. If a star wants to become a black hole after its death, then it requires at least 2 to 3 times the mass of our sun. If the star gravitational pull destroy the rest of the forces acting on it, and the remaining particle collapsing into a single point of infinite density is called the singularity.

From a distance, black holes behave in a simple and predictable way. We can consider them as a single point with mass and compute their gravitational effects on other objects by using a simple formula and Newtonian mechanics work.

### How to use the Black Hole Collision Calculator?

By using the simple Black Hole Collision Calculator, we can calculate what would happen when a black hole collides with any object in the universe. We have to know the mass of the black hole and mass of the object that is being eaten and the event horizon radius.

Provide all these values in all the input fields and click the calculate button to know the black hole gained mass, event horizon radius after the collision, event horizon growth and amount of released energy.

Some ranges of masses expressed in relation with the mass of the sun is along the lines:

1. Super Massive Black Holes: ~1-1000 million Msun
2. Intermediate Black Holes: ~10-1000 Msun
3. Stellar Black Holes: ~1-10 Msun
4. Neutron stars: ~ 1.5 Msun
5. Stars: ~0.5-250 Msun
6. Planets: 0.5 Msun

### How to see Black Holes? | The event horizon of a black hole

The event horizon is an imaginary line that divides what we can possibly see from what we cannot. To escape from an object gravitational field, you have to move to the opposite direction of the object attraction. The escape velocity is the velocity that should start with to escape from the attracting object surface.

If an object has the highest escape velocity than the speed of light, then not even light can escape its gravitational pull. It means that the object will appear black. As we know that black hole is treated as a point in space and its escape velocity is greater than the light speed. This limit or point of no return is called the event horizon.

Generally, we can't see the black holes but we can see the existence of their effects on the objects. The two main different types of interactions between a black hole and other objects are destructive and non-destructive. In this type of interaction, astronomers can observe a set of objects that are orbiting around nothing which is having a strong gravitational pull. So, it is the black hole. We can see the black hole with its existence because of the way other objects react to its presence.

The violent kind of interaction is also due to gravity, but the objects involved get a little too close to the black hole and end up being swallowed by it. From earth, we can see the bright flash of light coming from what is a dark spot.

### How Do Black Holes Eat Objects?

When an object falls into a black hole, a huge amount of energy is dispersed into the universe. The amount of energy in the flash of light changes from 3% to 42% of the mass of the object based on the black hole properties it falls into. One of the common ways it happens is the tidal disruption event.

When a star gets closer to a black hole, its parts are attracted by the different strengths causing the star to be torn apart. The parts of the star are detached from it and star spiraling with the black hole before being eaten. After a black hole is stucked in a star, it gains the star mass to increase its size or Schwarzchild radius or event horizon.

The increase of mass depends on the energy liberated during the merging proess. The released energy comes from the falling object's mass. The relation is explained with Einstein's formula i.e E = mc2. The amount of energy released depends on the initial approximation, mass of the falling objects and so on.

Physicscalc.Com has got concepts like friction, acceleration due to gravity, water pressure, gravity, and many more along with their relevant calculators all one under one roof.

### FAQ's on Black Hole Collision Calculator

1. What happens if 2 black holes collide?

When two black holes collide or merge to form an intermediate-mass black hole. When they collide, they produce ripples or waves throughout the space known as gravitational waves.

2. Can a black hole die?

The black hole is an area in the universe where gravity is so strong so that even light can escape from it. These are the most important objects in the universe. Black holes will die one day. When they do so monsters won't go gently into the night.

3. How to calculate the black hole lifetime?

The lifetime of a black hole can be calculated using the formula t = (M/MΓèÖ)3 x 1.160 x 1067 years. Here MΓèÖ value is 1.989 x 1030 kg and M is the mass of the black hole. Substitute the mass value in the formula and solve to get the black hole lifetime value.

4. What is the formula for the Schwarzschild radius of a black hole?

The Schwarzschild radius of a black hole formula is R = 2GM/c2. Where M is the mass, G is the gravitational constant and c is the speed of light. The Schwarzschild radius is the radius below which the gravitational attraction between the particles of a body must cause it to undergo irreversible gravitational collapse.