Can any object be compressed to a certain extent and converted into a black hole?

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Yes, we can make it, but so much developed technology has not been developed yet.

But the black hole we make will be destroyed very soon due to the hawking radiation coming out of the black hole.

First of all, we know how black holes are formed

Krishna holes (black holes) means black holes are objects with very high density and mass, which are very small in size. The gravity inside it is so strong that rays of light are impossible to get out of its clutches. Since it absorbs rays of light, it remains invisible.

In the year 1783, Professor John Mitchell of the University of Cambridge put forth his views regarding the black hole. After Michel, in the year 1796, French scientist Pierre Simon Laplace discussed the black hole in detail in his book The System of the World.

How are black holes formed?

It is necessary to understand the evolution of stars in order to know how a black hole is formed. In fact, the evolution of the star begins with a very massive cloud of dust and gases present in the galaxy, called Nebula. The amount of hydrogen inside the nebulae is the highest and contains 23 to 28 percent helium and a small number of heavy elements.

The density of the cloud increases when filled with gas and dust. At that time, the cloud starts to shrink due to its own gravity. Along with the contraction in the cloud, the temperature and pressure of its center also increase. Eventually, the heat and pressure become so high that the nuclei of hydrogen begin to collide and form the nucleus of helium.

In this case, Thermo-Nuclear Fusion starts inside the wires. This reaction inside the stars is similar to a controlled hydrogen bomb explosion. In this process, energy is produced in the form of light and heat. In this way, that cloud becomes a star shining with heat and light. The strong heat produced by thermodynamic fusion keeps the gravitational balance of the stars, with the star remaining stable for a long time. Ultimately, when the hydrogen and other nuclear fuels within the star are exhausted, they are not able to get enough heat to balance their gravity. In this case, the star starts to cool down.

In the year 1935, Indian astrophysicist Subrahmanyan Chandrasekhar made it clear that stars with a mass 1.4 times the mass of their depleted solar mass could not sustain themselves against their own gravity. An explosion occurs inside that star, which is called a supernova explosion. If its residue survives after the explosion, it becomes a highly denser 'Neutron star'.

This image is intended to explain the distortion caused by black holes in the time interval, but black holes are not of this size.

There are many stars in the galaxy whose mass is more than three-four times the solar mass. Due to excessive gravitational drag on such stars, the star starts to compress, and the space-time begins to distort, as a result when the star narrows to a certain critical limit and turns towards K tilts the time period so much that it becomes invisible. These are the invisible bodies which we now call 'Krishna Vivara' or 'Black Hole'. American physicist John Wheeler first used the term 'black hole' for these bodies in 1967.

If the density of the earth's material becomes millions of millions of times and its size is reduced to 1.5 centimeters, then in such a state, due to the strong gravitational force, the earth will not be able to emit light rays and it becomes a black hole. Will go. Density is more important than mass in any black hole. If the Sun is compacted and its radius of 700,000 kilometers is changed to 3 kilometers, it will result in a black hole. We know that it is impossible for the Earth and the Sun to shrink in this way because neither the mass of the Earth nor the force of gravity is so high nor that of the Sun.

Features of a black hole:

Black weaver size

The entire mass of a black hole is centered in a point called the Central Singularity Point. Scientists have conceived a circular boundary around the singularity point, often called the Event Horizon. Beyond the event horizon, all matter including light is attracted to the singularity point and pulled away. But no object can come out through the event horizon. The radius of the event horizon is known as the Schwarzschild Radius, named after the German scientist and mathematician Karl Schwarzschild.

Interestingly, Karl Schwarzschild himself disproved the physical existence of the black hole after it proved in principle. However, Carl Schwarzschild and John Wheeler are credited with the discovery of the black hole.

Albert Einstein According to Albert Einstein's Theory of Special Relativity, for an observer located at a certain distance, clocks near a black hole will run at very slow speeds. Time is relative according to special relativity theory. Time is subjective, the time when observers say 'now' applies only to the local system of instruction, not to the entire universe! This effect is called Time Dilation.

Due to the gravity of the black hole, any observer far away from it will see that any object falling inside the black hole is falling very low near its event horizon, reaching it seems to take an eternity. it occurs. At that time all the activities of that object will start to be very slow, so the light of the object will appear to be very red and blurred (unclear).

This effect is called Gravitational Red Shift. Eventually, the object falling inside the black hole will become so blurred that it will stop appearing. Mostly, people are of the opinion that the black hole behaves like a vacuum cleaner, but it is not so. Whatever will go near the black hole will swallow it. This means that if our Sun becomes a black hole, then its radius will be 3 kilometers, even then the orbits of all the planets will be completely unchanged. A black hole will not be able to swallow any planet, provided it does not come close to the black hole.

There are many types of black holes in the universe which are identified by their specific physical properties. Stars whose mass is slightly more than the solar mass and due to gravitational contraction, they eventually turn into a black hole. Such Krishna particles are called Stellar Mass Black Hole. Black holes that form in the center of galaxies are called Super Massive Black Hole. Their mass is millions of millions more than the solar mass. According to scientists, there is a huge black hole in the center of our Milky Way Milk Milkhala and its mass is 10 million times the solar mass.

Black holes whose mass is less than the solar mass are formed not by gravitational contraction, but because of compression of the matter in its center due to pressure and heat. Such Krishna holes are known as Primordial Black Hole or Small Black Hole. Scientists believe that these miniature Krishna holes may have been formed at the time of the creation of the universe. According to physicist Stephen Hawking, we can find out a lot about the early stages of the universe by studying such black holes.

Some black holes also rotate at a fixed speed on their axis. In the year 1963, Roy Kerr, a New Zealand mathematician and scientist, provided the mathematical basis for the existence of these rotating black holes. The size of these Krishna vivas depends on their rotation rate and mass. Scientists now address such Krishna holes as Kerr's Black Hole. Their structures are very complex, and event horizons are also spheroid. Black holes that do not rotate are called Schwarzschild Black Hole.

How to find a black hole?

As we know that black holes do not emit rays of light, how can we expect to find them? This was previously a serious problem for astronomers. But astronomers also found a solution to this problem. According to Mitchell, black holes have the effect of gravity on objects near them even when they are invisible. Under this project, astronomers observed pairs of stars in the sky, which bound each other by gravity and orbiting each other. Imagine two stars in the sky orbiting each other, one of them is invisible and the other is visible. In such a situation, the visible star will orbit the invisible star.

If you consider an invisible star in a hurry to be a black hole, then you can be wrong because it can also be a star that is far away from us and its light is so slow that we...

If you hastily consider an invisible star as a black hole, you may be mistaken as it may also be a star that is far away from us and its light is so slow that we cannot see it. If astronomers collect information related to its mass on the basis of astronomical calculations related to the orbit of the visible star, it can be easily detected by astronomical methods about the mass of that invisible star. If its mass is three to four times the solar mass, it is highly likely that the invisible star is a black hole.

There is also another way to prove the existence of black holes. Imagine that there is a visible star near the black hole, then the black hole will continue to drag the gaseous mass of this visible star from its backside into its own. Due to the loss of visible star matter in a black hole, X-rays will be emitted at a much faster rate (due to friction, heat, and pressure). Then by observing and studying the origin of X-rays the physical existence of a black hole can be proved.

Seagnus X1: This will look like in visible light. This Shyam Weaver is drawing the mass of his companion star, creating an accretion disc. The gas in this disc is hot, emitting X rays.

In the year 1965 astronomers found an extremely intense X-ray source in the Hans_Cygnus planetarium. That source was named Cygnus X-l. In 1970, it was discovered by a US-launched satellite that Cygnus X-1 is not a white Vamana or a neutron star, but a black hole. Actually, Cygnus X-1 is a pairing asterisk. The visible star of this pair of stars is very large, orbiting an invisible star. Astronomers have determined the mass of Cygnus X-1 to be equal to the mass of six suns by astronomical methods. This makes it clear that Cygnus X-1 is a black hole.

Stephen Hawking and the Black Hole

Our current understanding of black holes is based on the work of physicist Stephen Hawking. Hocking published a paper in the year 1974 titled Black Holes Not So Black. In this paper, Hawking demonstrated that black holes are not completely black, but emit small amounts of radiation, based on the principles of general relativity and quantum physics. Hocking also demonstrated that the radiations emitted from a black hole are ejected due to quantum effects. This effect is known as Hawking Radiation.

Black holes gradually lose their mass due to the Hawking radiation effect and also cause energy loss (E = mc²). Ultimately, the black hole evaporates after this process lasts for a long interval. Interestingly, supermassive black halls emit small amounts of radiation, while small black holes emit very fast radiations to form vapors.

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