Black Hole Spin Speed: Scientists have discovered how fast a supergiant black hole rotates on its axis. Know what is the spin speed of a black hole.

Supermassive Black Hole Spin: Scientists have calculated the spin speed of a black hole for the first time. Spin speed means how fast the black hole rotates on its axis. Astronomers at the Massachusetts Institute of Technology (MIT) had set their sights on a supermassive black hole one billion light years away from Earth. When the black hole woke up and ate, a change in the brightness of the light was seen. This change was caused by a disk of matter that rotated and wobbled. According to Dheeraj Pasham of MIT, this wobble helped his team tell the spin speed at the center of the black hole. What was the speed of rotation of the black hole on its axis? The answer is- less than one-fourth the speed of light. This speed is very low for a black hole from which even light cannot escape! Pasham said that this discovery of scientists will be useful in future.

The MIT scientist said, ‘By studying many black hole systems in this way in the coming years, astronomers can get an estimate of how much difference there is in the spin speeds of black holes. This may also help them understand how black holes have evolved.

Supergiant black hole: the biggest mystery of the universe

Supergiant black holes are found in the centers of galaxies. Their mass can be billions and trillions of times that of the Sun. These supermassive black holes, which contain the immense power of gravity, hold the galaxies together. Scientists believe that the central black hole plays an important role in the structure and evolution of the galaxy.

Black holes themselves do not produce light. Their density is so high that the speed required to escape from the black hole’s gravitational force is much greater than the speed of light in vacuum. The light around a black hole comes from the accretion disk dancing around it. This disk of matter and gas becomes the food of the black hole

There is nothing in the Universe more awe inspiring or mysterious than a black hole. Because of their massive gravity and ability to absorb even light, they defy our attempts to understand them. All their secrets hide behind the veil of the event horizon

Recent findings indicate that a supermassive black hole is spinning at less than 25% the speed of light. This is a slow speed for a black hole, which can spin at up to 94% the speed of light

The researchers took this pattern of wobbling and worked it into the original theory for Lense-Thirring precession. Based on estimates of the black hole’s mass, and that of the disrupted star, they were able to come up with an estimate for the black hole’s spin — less than 25 percent the speed of light

All black holes have spin, which they develop through their interactions with other matter in space. When black holes grow by accreting matter, they can spin to greater speeds; when they grow through mergers with other massive objects, they tend to slow down. In its recent work, the team managed to deduce a supermassive black hole’s spin by measuring the wobble of its accretion disk after a star has been disrupted—a polite word for torn up—by the gigantic object. They found the black hole’s spin was less than 25% the speed of light—slow, at least for a black hole. The team’s research was published today in Nature.

The MIT scientist said, ‘By studying many black hole systems in this way in the coming years, astronomers can estimate how much the spin speed of black holes varies. It may also help them understand how black holes evolve. Supermassive black holes are found in the centers of galaxies. Their mass can be billions and trillions of times that of the Sun. These supermassive black holes, with their immense gravitational power, hold the galaxies together. Scientists believe that the central black hole plays an important role in the structure and evolution of the galaxy.

Black holes themselves do not produce light. Their density is so high that the speed required to escape the black hole’s gravitational force is much greater than the speed of light in a vacuum. The light around a black hole comes from the accretion disk dancing around it. This disk of matter and gas becomes the food of the black hole

Black holes are one of the strangest things in the universe. It seems they don’t make any sense. This is an enormous amount of matter packed into a minimal area. To better understand, think of a star ten times more massive than the Sun packed into a sphere roughly the size of New York City. The result is that the gravitational field becomes so strong that even light cannot come out. Because no light can escape from black holes, they are invisible. Finding black holes requires a space telescope with special instruments. These help us see how stars near a black hole behave differently than other stars

How are blackholes formed

A collection of giant hydrogen atoms forms a star. At their core, hydrogen atoms fuse into helium, releasing enormous amounts of energy. Free energy, in the form of radiation, pushes against gravity and maintains a delicate balance between the two forces. A star remains fairly stable as long as fusion occurs at its core. In stars much more massive than the Sun, the heat and pressure in the core allow them to fuse heavier elements until they form iron. Iron continues to accumulate in the center of the core until it reaches a certain critical point, and suddenly, the balance between radiation and gravity is broken. The result is that the core collapses and explodes in on itself. Moving at about a quarter the speed of light, it packs even more mass into the core. It was at this moment that all the heavy elements in the universe were created. As stars die in supernova explosions, they turn into either neutron stars or black holes, depending on the mass of the star.

types of black holes

There are four types of black holes:

stellar
intermediate
giant
Small
The most commonly known method of black hole formation is stellar death. As stars reach the final stages of life, most of them will lose mass, swell and cool to become a white dwarf. But the largest of these, ten times or 20 times more massive than the Sun, are destined to become either super-dense neutron stars or stellar-mass black holes.

Why do stars end up as blackholes

The answer involves gravity and internal pressure within the star. These two things oppose each other – the star’s gravitational force acting on a piece of matter on the surface of the star will tend to cause that matter to fall inward, but the internal pressure of the star, which acts outward on the surface, will Is happening, would like so that the matter flies outside. When these two are balanced (ie equal in strength) the star will maintain its shape: neither collapsing nor expanding. At present this is the situation for the Sun, and even for the Earth.
However, when a star runs out of nuclear fuel, and so continues to lose energy from the surface (it is emitting light energy), while not replenishing the energy lost through nuclear fusion (no longer nuclear fuel) If it is doing so, gravity will overcome the internal pressure and the star will either slowly contract or rapidly collapse, depending on the details of the internal structure and composition. Gravity overcomes the internal pressure of the star, because that pressure was generated by a normal, hot gas, and that gas is losing energy as the star emits energy from the surface.

Thus the star may end up as a black hole. It just depends on whether another source of pressure (other than that generated by the normal, hot gas) becomes strong enough to balance the gravitational force inward, causing the collapse to some smaller size. Is it stopped or not? Apart from the pressure generated by hot gas, there are other forms of pressure. Pressing your hand on the desk top will cause you to experience one of these other pressures—the desk pushes against you, in fact it can support your weight (the force of gravity)! The pressure that keeps the desk rigid against your weight is caused by forces between the atoms in the desk.

Furthermore, electrons within atoms must avoid each other (for example, they cannot all be in the same atomic “orbit”—this is called the “exclusion principle”). So, if we had a collection of freely moving electrons they would also avoid each other: the more you compress the collection (the smaller the volume they are confined to) the more they rebel against the squeeze. Do – A pressure opposes the binding of your electron.

This “electron avoidance” pressure can only be strong enough to resist gravitational forces within a star equal to the mass of the Sun, when the star is compressed by gravity to about the diameter of the Earth. Thus a massive star like the Sun is prevented from becoming a black hole when it collapses to the size of Earth, and the internal “electron avoidance” pressure (called “degenerate electron pressure”) becomes strong enough to hold the star. . Above. This type of pressure does not depend on the energy content of the star—-even if the star continues to lose energy from its surface, the pressure will sustain the star. Our Sun can never become a black hole.

However, if the star is more massive than something like 3 to 5 solar masses, its gravitational force will be large, and its internal degenerate electron pressure will never be enough to prevent its collapse. It turns out that neutrons can also obey the exclusion principle and that neutrons will be produced in abundance when a massive star collapses, but even neutron degeneracy cannot prevent the collapse of massive stars — 3 to 5 Nothing more than the solar mass can be stopped and it would become a black hole according to current thinking.

How does time change in blackholes

Well, in a certain sense it hasn’t changed at all. If you enter a black hole, you will find that your clock is ticking at the same speed as it always has (assuming both you and the clock survived the black hole). However, you will fall rapidly towards the center where you will be killed by massive tidal forces (for example, the force of gravity on your feet, if you fall feet first, will be much larger than on your head, and you will fall apart. ) ).
Although the ticking rate of your watch as you observe it will not change, as in special relativity (if you know anything about it), someone else will see a different ticking rate than usual on your watch, and You will notice their clock ticking at a different rate than normal. For example, if you position yourself just outside the black hole, you will find that your clock is ticking at a normal speed, but you will notice that a friend’s clock at a great distance from the hole is ticking at a much faster rate. It is ticking. than yours. That friend will see his watch ticking at a normal speed, but his watch will tick very slowly. Thus if you stayed outside the black hole for a while, then went back to join your friend, you would find that the friend had grown older than you during your separation.(will an observer falling in blackholes can see the future events)

The common presentation of these gravitational time dilation effects may lead one to wrong conclusions. It is true that if one observer (A) is stationary near the event horizon of the black hole, and another observer (B) is stationary at a considerable distance from the event horizon, then B will see A’s clock ticking slowly, and A will see B’s watch moving faster. But if A falls toward the event horizon (eventually crossing it) while B remains stationary, then what each sees is not as straightforward as the above situation suggests.
As B sees things: As A falls toward the event horizon, the photon from A takes longer to get out of the “gravity well”, causing A’s clock to noticeably slow down, as seen by B. goes, and when A is on the horizon, any photon emitted by A’s clock takes (formally) infinite time to reach B. Imagine that each individual clock emits a photon for each tick of the clock, to make it easier to think about it. Thus, as you say, A appears to freeze, as seen by B. However, A has crossed the event horizon! It is merely an illusion (literally an “optical” illusion) that causes B to think that A never crosses the horizon.

As A sees things: A falls, and crosses the horizon (probably in a very short time). A sees that B’s clock is emitting photons, but A is moving away from B, and so is never able to collect more than a finite number of those photons before they cross the event horizon. (If you prefer, you can think of this as the cancellation of gravitational time dilation by the Doppler effect—causing A’s motion away from B). After crossing the event horizon, photons coming from above are not easily resolved by the origin, so A cannot figure out how B’s clock kept running.

A finite number of photons were emitted by A before crossing the horizon, and a finite number of photons were emitted by B before A crossed the horizon (and were collected by A).

You might ask what would happen if A were brought down so slowly toward the event horizon? Yes, the Doppler effect will not apply unless, at some practical limit, A gets very close to the horizon and cannot avoid falling. Then A will see just as limited a total of photons as B (but now a larger number—covering more of B’s ​​time). Of course, if A actually “hangs” long enough before falling, then A can see the future of the universe.

Bottom line: Falling into a black hole alone won’t give you a view of the entire future of the universe. Black holes can continue to exist without being part of the Ultimate Big Bang, and matter can fall into the black hole.

For a very good discussion of black holes for non-scientists, see Kip Thorne’s book: Black Holes and Time Warps.

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