2020년 9월 3일 목요일

10.03 - 중력복사(Gravitational Radiation)

10.03 - 중력복사(Gravitational Radiation) [커세라 강의 페이지]



One of the foundational principles of special relativity is that light always travels at the same constant speed. The speed of light is fast, but it still takes 8.3 minutes to travel the enormous distance from the Sun to the Earth. This means that if the sun were just suddenly change brightness, there would be a delay of 8.3 minutes before we would see the change here on Earth.

특수 상대론의 주장중 하나가 빛의 속도는 불변이다. 태양에서 불발한 광자가 지구에 도착하는데 8.3분 걸린다.

Suppose that powerful aliens with advanced technology managed to change the Sun's gravity, maybe by removing a big blob of hot gas.

어느 발전된 외계인이 태양의 가스 일부를 날려버렸다고 하자.


Removing the gas also causes the Sun to dim at the same time. If we calculate the gravitational traction between the Sun and the Earth.

태양은 질량이 줄어들고 아울러 빛도 약해진다.

Newton's equations had no time dependents. If the sun's mass suddenly changes as it were, if aliens removed a large portion of gas. Newton would have predicted that the earth would feel a different force due to gravity instantaneously, with no delay.

뉴튼의 만유인력 법칙은 시간 의존성이 없다. 태양의 질량이 줄어듬과 동시에 지구에서 만유인력이 변했다는 것을 알아챌수 있다.


If gravity changes instantaneously, as Newton predicted, it would still take the photons emitted by the Sun 8.3 minutes to reach the Earth, revealing the alien's actions as the Sun becomes dimmer. This means that we could receive information about changes to the Sun at a speed faster than light by using gravity. This instantaneous transmission of information is sometimes called action at a distance.

태양의 중력이 변했더라도 빛을 발할 테고 광자가 지구까지 도달하는데 여전히 8.3분 걸린다. 외계인이 태양을 어둡게 만들었다는 사실은 8.3분후에 알아 채게된다. 뉴튼의 만유인력은 태양질량이 줄어든 사실을 빛보다 빨리 알 수 있다는 뜻이기도 하다. 뉴튼은 이렇게 즉각적인 정보전달을 멀리있는 변화(action at a distance)라고 했다.


Einstein realized that Newton's theory of gravity was wrong because it implies that action at a distance takes place and that gravity could transmit information faster than the speed of light.

아인슈타인은 뉴튼의 이론에 의문을 제기했다. 중력 변화가 빛보다 빠르게 전달 될 수는 없기때문이다.


Although there were no experiments Einstein could conduct that show that action at a distance is incorrect, Einstein knew that it would imply that there could be ways to transmit information at speeds faster than light which would contradict the principles of special relativity.

아인슈타인은 실험으로 증명할 수는 없지만 빛보다 빠르게 정보가 전달 될 수 있는 원인은 다른데 있을 것이라고 생각했다.

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Einstein theorized that gravity could be made compatible with special relativity if changes in gravitational fields are transmitted by gravitational waves that obey the speed of light limit in the universe. Gravitational waves, also called gravitational radiation, are an important part of Einstein's general theory of relativity.

아인슈타인은 빛의 속도에 관한 특수상대론에 배치되지 않으면서 중력에 관한 이론을 세웠다. 중력장의 변화에 의해 발생하는 중력파 혹은 중력복사는 우주의 기본 원칙인 빛의 속도 한계를 따른다는 것이다. 일반 상대론의 중요 부분중 하나다.


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Let's return to the aliens who are changing the Sun's mass and brightness. Einstein theories predicts that it takes 8.3 minutes for the gravitation force felt by the Earth to change, so changes in gravity travel at the same speed as light.

The relationship between the force of gravity and gravitational radiation is similar to the relation between electrostatic forces and the emission of electromagnetic radiation or light.

중력과 중력파의 관계를 정전기력과 전자기파의 관계와 같다고 이해해보자.

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An electron or a proton are just two examples of charged particles, which create an electrostatic field. Electrostatic fields can be attractive if the force is between opposite charges, or repulsive if the force is between same charges.

전자나 양성자는 하전된 입자다. 전정기 장은 하전된 입자 사이에 작용하는 인력 혹은 척력이다.

By grabbing a balloon against your head you cause negative charges or electrons from your hair to migrate to the balloon, leaving your head positive charges. If you then hold the negatively charge balloon near your positively charged head your hairs would stand up. Following electrostatic field lines.

The word static, means that the system doesn't change with time. Positive charge, like some hair, will feel and attractive electrostatic force that will feel a force toward the negatively charged balloon. The electric field of the balloon influences nearby objects, but in a static system, there is no electromagnetic radiation or light emitted in this situation.

'정(static)'이라는 말은 시간의 변화를 고려하지 않은 시스템이라는 뜻이다. 전하들이 전기장을 형성하여 인력 혹은 척력을 발휘하지만 복사가 잃어나고 있지 않다.

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If we want to produce electromagnetic radiation, we need to create periodic changes in the static charges. This can be accomplished by changing the position of a charged balloon, say by waving it back and forth rapidly. Positively charged hair will be attracted first in one direction, then the other, and so on. This is situation which produces a time changing electric and magnetic field that causes a disturbance called electromagnetic radiation, also known as light.

전자기 복사를 일으키려면 정전하들이 주기적으로 변해야 한다[위치 혹은 전하량]. 머리를 문지른 풍선을 한 방향에서 주기적으로 흔들면 전기장이 흔들리고 이로인해 자기장이 생겨 전자기 복사(방출=radiation)이 일어난다.

For example, if the balloon is moved back and forth once per second, it generates a changing electric field that moves away from the source at the speed of light. One complete cycle of the balloon corresponds to one cycle of the light wave. So if the balloon moved at one hertz, it produces a photon with a wave length equal to the distance light travels in one second. That's 299,792 kilometers of photon at the very long end of the wave length spectrum in the radio frequencies.

예를 들어 머리에 문지른 풍선을 1초에 한번씩 움직이면 1헤르츠짜리 전자기파가 방출된다. 아주 파장이 긴 빛이다. 이 빛도 속도는 299,792 킬로미터다.
 
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This electromagnetic wave travels at the speed of light perpendicular to the motion that the balloon is being waved. Information about the changing balloons position reaches your hair after a time equal the distance divided by the speed of light. When the wave passes by a charged particle, the particle will feel a time changing force. That will cause it to oscillate back and forth in a direction perpendicular to the direction the wave travels in.

Normally, we don't use balloons to create electromagnetic waves. Instead, we might have an alternating current traveling through a dipole antenna to create radio waves, a long wavelength form of light.

The important thing to know is that light is only emitted when there are time-changing electric charges or magnets.

중요한 점은 빛은 전하나 자기가 시간 변화를 일으킬 때 빛의 복사가 발생된다는 점을 기억해 두자.

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A star or planet has a gravitational field that doesn't change with time, and unlike electrostatic forces, gravity is only attractive. A small mass place near a heavy planet will feel an attractive gravitational force that will pull it towards the surface. If there is no motion of the masses, there will be no gravitational radiation emitted. Just like the electrostatic example, in order to excite gravitational waves, we're going to need a gravitational field that changes with time.

중력은 끄는 힘만 있다. 그래서 만유인력이다. 두 질량체의 질량변화가 없다면 인력은 존재하나 중력 복사는 없다. 전자기파와 마찬가지로 중력파가 나오려면 질량에 시간 상 변화가 있어야 한다.

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When gravitational waves are created, they move away from their source at the speed of light and, as the wave moves. It distorts space time by stretching and compressing spacial dimensions periodically in the two directions perpendicular to the direction that the wave travels.

생성된 중력파는 전자기파와 마찬가지로 빛의 속도로 움직인다. 시공간이 압축과 이완을 시간상 주기적 변화를 일으키면 중력변화의 수직방향으로 파동이 전달된다. [전자기파의 이동방향은 전자기장의 변화에 대해 수직이다.]

These waves are called transverse waves and can be understood in a simplified sense by the analogy of a transverse wave on this rope that Curtis and Ross are playing with. In this video, we see Ross waving the rope up and down, which is sort of like a gravitational wave source. The wave travels along the rope horizontally from left to right and then from right to left. At each point between Ross and Curtis, the rope is forced to move up and down at the same frequency as Ross's hand.

In a transverse wave, the movement of the medium is in a different direction than the direction that the wave travels in. A gravitational wave is a wave in space-time, which means that instead of moving objects a gravity wave compresses and decompresses space-time.

중력파는 횡파(transverse wave)인데 파동의 진행과 메질의 진동이 서로 수직이다. 중력파는 시공간에서의 파동 물체의 움직임 대신 시공간이 앞북되었다 이완되기를 반복한다.

Suppose that a gravitational wave travels from the ceiling to the floor through my body. Focus on my arms. The affect of the gravitational wave will be to stretch one arm out outwards and compress the other arm inwards. Then the second part of the wave's periodic motion will cause the opposite changes in each arm. Periodic motions of my arm will then occur when the wave travels through my body.

If a gravitational wave were to pass by your ear, it would cause your eardrum to start vibrating, so that you could in principle hear a gravitational wave if you had sensitive enough ears. For this reason, scientists often convert gravitational waves into equivalent sound waves, which is how we got the chirp sound of two merging black holes.

중력파가 사람의 기를 통과하면서 고막을 두드린다. 고막이 충분히 민감하다면 중력파 소리를 들을 수도 있다. 과학자들이 두 블랙홀이 충돌하면서 생성되었던 중력파를 엄청 증폭해서 들려주는 소리를 들어봤을 것이다.


In reality the wave are very weak and changing arm lengths are microscopic. In the Star Trek: The Next Generation episode called Hero Worship, the Enterprise is violently rocked by gravitational waves. This is rather difficult to understand since in reality the waves are very weak, and the Enterprise would have had to have been right next to a ridiculously strong explosive event, in order to get such a strong rocking event.


Scientists on Earth have been working hard for decades to build detectors, sensitive enough to detect gravitational waves, and directly detected them for the first time in 2015.

과학자들이 지난 수십년간 각고의 노력끝에 2015년 처음으로 미세한 중력파를 감지해 냈다.

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[인터뷰] [커세라 페이지]

How do binary pairs of black holes form?
Interview with Dr. Tyrone Woods, Researchers at Monash University

So I think something that is fascinating everybody in the Black Hole community right now is the recent discovery by LIGO, demonstrating the existence of binary pairs of black holes. How these objects actually form still remains a mystery, although we have a lot of ideas.

Generally, one major picture is that a pair of stars born together eventually die together, one forming a black hole and then the other.

Another idea is that to get around some of the complicating factors in terms of trying to actually make a binary pair of black holes together starting from scratch is to form these objects initially born separately in a globular cluster, a very dense system of stars. And then many of which orbit our own Milky Way.

These are sort of the building blocks of galaxies. These systems move around within their den system and interact far more often than they would in a lower density stellar environment like our Milky Way. And they can swap partners and maybe in this way bring together two black holes in a close enough orbit that they eventually merge but we don't know which is the right answer.

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10.02B - 중력렌즈 현상: M87의 블랙홀 (Gravitational Lensing: The Black Hole in M87) [커세라 강의 페이지]

Our home galaxy, the Milky Way, is located in a small group of about 30 galaxies known as the Local Group, for lack of a better name. Groups of galaxies with more than hundreds or thousands of galaxies are known as clusters. The Virgo cluster of galaxies located 65 million years away from us has over 2,000 member galaxies.


Deep in the heart of the Virgo cluster of galaxies, an enormous black hole hides inside the largest galaxy in this cluster. This giant elliptical galaxy is named M87. It has a mass that is about 10 times larger than the Milky Way.


Images of the galaxy M87 show a long jet that is thousands of light years long, reaching out from the central region of the galaxy. This jet led astronomers to suspect that a supermassive black hole lies at the center of the galaxy.




In 1994, the then new Hubble Space Telescope was pointed at the nucleus of M87. At the core of the galaxy, the telescope was able to resolve a disk of gas, suggesting orbital motion around the galaxy center.


Hubble spectrograph was able to detect Doppler shifts and emission lines on either side of the disc at distances of 60 light years from the galaxy center. The red-shifted and blue-shifted spectral lines allow the measurement of the gases velocity, which was then used with Kepler's laws to find the mass of the center.


The resulting mass of 2.5 billion solar masses is large enough that the only sensible conclusion is that a supermassive black hole lies at the center of this galaxy.

허블 망원경으로 제트를 관측하고 분광 측정으로 강착원반의 적색 편이와 청색 편이를 측정하여 M87은하의 중심에 거대 블랙홀이 존재한다는 확신을 가졌다. 케플러 법칙에 따라 회전하는 (강착원반의) 가스구름을 계산해보니 질량이 태양의 25억배에 이르는 초거대 블랙홀이 중심에 있는 것으로 추정되었다.  

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Back at this time, I was a student studying black holes, so it was really exciting to hear about this observational confirmation of the existence of supermassive black holes.


The gigantic mass of the black hole, and the relatively close distance on astronomical scales led the Event Horizon Telescope team of scientists to choose the black hole in M87 as their first target. In April 2017, they pointed radio telescopes located on multiple locations on the earth at M87.



The black hole at the center of the galaxy M87 is sometimes called M87 star. More recently, it has been renamed Powehi, which is a Hawaiian name, meaning the adorned, fathomless dark creation.

After two years of data analysis, they announced their results and images in April 2019. The orange donut image swept the Internet by storm. But what is this image actually showing us?


The Event Horizon Telescope observes radiowaves. So the orange color is a false color image that maps the brightest radio waves to yellow and dimmer radio waves to dark orange. The astronomers could have shown this picture in black and white, but the use of color does help bring out details to our eyes.


This set of images shows how the image of the black hole changes day by day. The general shape of a photon ring that is bright on one side and dim on the other, surrounding a black region known as the black hole shadow, stays constant. But you can see that the ring develops little bumps that move around a bit on timescales of days.

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The ring-shaped comes about as photons travel around the black hole on curved paths. A bright region on the far side of the black hole will emit light that travels around the black hole to the earth. Since the light can travel over, under, or beside the black hole, we see a ring of light surrounding a dark region.


The outer edge of the black hole shadow has radius, R_shadow is equal to the square root of 27 times GM over c squared, which is about 2.6 times the event horizon radius of a Schwarzschild black hole.


Measuring the size of the image allows an independent measurement of the black hole's mass.

위의 블랙홀 그림자의 반경은 블랙홀 질량 추정치와 별도로 관측 영상만으로 계산된 관측 추정치다.

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The Doppler-boost effect is responsible for the bright and dim region seen in this image. Regions of gas that are moving towards us are blue-shifted and appear brighter, while regions that are moving away from us are red-shifted and appear dimmer to us.


The astronomers computed thousands of model accretion disks, traced the light rays around the black hole, and produced images similar to this one.

Then the blurring effect of the gas between the black hole and the earth was added to the simulated image.

The simulated blurred image is then compared to the observed image in order to validate the physical interpretation of the image. This is a really remarkable observation and analysis.


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The next black hole that the Event Horizon Telescope collaboration plans to observe is Sagittarius A star, the supermassive black hole at the center of the Milky Way.

국제공조를 통한 EHT의 다음 관측 대상은 우리은하 중심의 초거대 블랙홀 궁수 A*다.
 


You might think that Sagittarius A star would be easier to observe than M87 star. The center of the Milky Way is 1,000 times closer to the earth than the galaxy M87, so surely the black hole shadow should look larger.


SGR A*는 M87보다 1000 배나 가깝지만,
 
However, the mass of Sgr A star is about 1,000 times smaller than M87 star's mass. This makes the event horizon and the size of the shadow smaller. The overall effect is that the shadow will appear to have a similar size.


크기는 1000분의 1에 불과하다.

The real problem is that Sagittarius A star is known to very rapidly on timescales shorter than a day. This will make the image jump around and blurry. The observation of our own black hole shadow will be even more difficult than the observation of M87 star's shadow.

게다가 M87이 (강착원반의) 광도변화가 수 일인데 비해 SGR A*의 (강착원반의) 광도변화는 매우 짧다. 이런 이유로 M87보다 관측이 매우 어렵다.

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10.02 - 중력 렌즈 현상(Gravitational Lensing)

10.02 - 중력 렌즈 현상(Gravitational Lensing) [커세라 강의 페이지]



When light enters glass, the direction that light travels, changes, or bends is a process called refraction. If the surface of glass is curved appropriately we produce a lens, which can magnify, diffuse, or distort the light rays from objects in the background.


Since gravity causes light to travel in curved spacetime, any object with a gravitational field appears to bend light as a gravitational lens.


The examples that we looked at earlier like this image of the Cheshire Cat galaxy group were cases where the light was emitted far from the closer lensing mass. In this image, the arcs making the smile and outline of the face are images of galaxies lying far behind the eyes and nose galaxies whose mass is warping space-time.


However, if we consider ultra dense stars with gargantuan gravitational fields, the light they emit will also travel on curved paths. Neutron stars are examples of stars with strong enough gravity that they exhibit gravitational lensing. Their emitted light travels part of the way around the star before it can escape to be observed by telescopes.

중성자 별 정도의 중력으로도 중력 렌즈 현상을 일으키는데,

By observing how light is bent around neutron stars we can understand the properties of these stars better which will help us keep from confusing neutron stars or black holes in the future.

중력렌즈 현상을 관측하여 별의 특성을 좀더 이해하는데 도움이 된다. 하지만 중성자별과 블랙홀을 구분을 혼란케하는 요인이기도 하다.

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If you look at my head, you can only see the front of my head and you have no way to know what the back my head looks like, unless I turned around. This is because in situations with weak gravity like here on Earth, light travels on straight paths from my head to the camera. But if my head was really heavy, so that my head had a gravitational field as strong as a neutron star then light originating from the back of my head will travel on a curved path around my head would be captured by the camera.

This would give you a distorted image of my face surrounded by all my hair. As a result, my head would look larger than it really is.

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This animation shows the effect of a neutron star's gravity on the light that it emits. In these cartoon animations, we show a dim star with one bright spot on it.

The left animation shows an image of a star as though it's gravity has no effect on the light that it emits. In this case, we see the hotspot for only half of the rotation period and it is eclipsed when it is on the back side of the star. Since the hotspot appears brighter than the surrounding star, a plot of the overall brightness would increase as the hotspot rotates into view and decreases as it becomes hidden again.

The right animation shows the same star, but now it includes the gravitational effects. The star's strong gravity causes the light emitted by the star to travel on curved paths so that parts of the star that would normally be hidden are distorted into view. The strong gravity allows us to see the bright spot all of the time even when it is on the back side of the star.

The star's gravitational field distorts the circular spot's image, so that it looks like a thin curve, and it allows us to see around the spin poles. Since the hotspot is now visible throughout the rotation of a star, there is much less variation in the overall brightness with time as shown on the graph below the animation.





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The star is rotating so fast that the equator is moving at 30 percent of the speed of light. When the spot is moving towards us, the light it emits is blueshifted, and when the spot is moving away from us, it is redshifted by the Doppler effect. When light is Doppler shifted, there is another relativistic effect called Doppler boosting which makes the blueshifted light appear brighter and the redshifted light appear dimmer.


If you pay attention to the brightness scale on the right, you'll notice that the spot is brightest when it is moving towards us and it is dimmest when it is moving away from us.

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NASA's NICER x-ray telescope is measuring the gravitationally lensed and Doppler boosted light from hotspots on neutron stars. NICER is attached to the International Space Station and observes X-rays emitted by neutron stars with spots as well as black holes.



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Black holes do not have a surface. So, we can't observe hot spots on rotating black holes in the same way that we observe them on neutron stars, but we do know that there are light emitting structures like accretion disks that orbit black holes. Images like this one drawn by artists represent accretion disks around black holes.


In most pictures, the artist has drawn the accretion disk as though the black holes gravity does not warp space-time or the paths that light rays follow. So, we see the accretion disk as flat. But if a neutron star's gravity can distort the paths of light, then a black hole's can too.

This vinyl record represents a crude model of an accretion disk, and the hole at the center represents a black hole. If we ignore the black hole's strong gravity then when you look at this disk the light rays travel from the disk to the camera on straight lines and the disk looks flat. A black hole with an event horizon with the same size as this hole has a Schwarzschild radius of 3.6 millimeters. This corresponds to a mass that is about half of the planet Venus squished into this hole.

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The strong gravity of the black hole will distort your image of the back of the disk, you will still see the front of the disk since the light rays don't have to pass by the black hole in order to get to the camera.

Light emitted by the back of the disk has to travel close to the black hole in order to get the camera. Light from the back is bent by gravity to travel up and over the black hole to the camera, as a result this back curve will appear to look like an arch over the black hole.


But the disk also has a bottom that emits light. Light emitted by the bottom can travel down and below the black hole to get to the camera. The bottom of the disk will look like a second arch below the black hole.

A more accurate drawing of an accretion disk around the black hole will show the disk arching over and below the black hole.

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The movie Interstellar features a view of a supermassive black hole with an accretion disk. The director, Christopher Nolan, wanted to have a fairly realistic view of the disk that includes gravitational lensing. So, he consulted physicist Kip Thorne, who recently shared the 2017 Nobel Prize in physics. The resulting image produced for the movie is shown here.

영화 '인터 스텔라'에서 묘사된 블랙홀

In this image, we can see the front of the disk, the top of the back of the disk, and the bottom of the back of the disk.

강착원반과 중력렌즈가 세밀하게 표현됐다.


However, the black hole created for the movie required some simplifications. First, they wanted a black hole that would be safe for the astronauts to visit. So, they did not include a jet. This suggests that Gargantua is not accreting enormous amounts of matter.

우주비행사의 안전을 고려해 제트 분출은 없는 것으로 했다. 이는 블랙홀 가르간츄아가 물질을 한없이 끌어당기지 않는 것으로 상정한 것이다.

They also chose a colder than usual accretion disk which is only a few thousand degrees Kelvin, so that emits ultraviolet visible and infrared light but practically no harmful X-rays.

또한 강착원반의 온도를 수천도 가량이라고 하여 위험한 X선이 방출은 없는 것으로 했다.

When we looked at the light from a rotating neutron star, we saw the Doppler boosting effect makes the blueshifted side of the star appear brighter than the redshifted side. The accretion disk orbit the black hole at high speeds. The side coming towards you is blueshifted and should appear brighter than the side moving away from you. The director was worried that people watching the movie might get confused if the Doppler boosting effect were included. So, they left it out from the rendering.

블랙홀 모습에서 반쪽만 보여줌으로써 도플러 부스팅 효과를 보여주지 않았는데 관객들의 혼란을 우려했다. 

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This computer animation shows the results of a magneto hydrodynamic computer simulation of an accretion disk around the black hole. The researchers are simulating realistic patterns in the disk which makes it easier to see the motion of the gas.

At the start of the animation we're looking down on the disk and then we move downwards so that we are viewing the disk from just above the plane of the disk.

[강착원반 시뮬레이션 평면도]

The warping effect of gravitational lensing becomes more apparent as we look into the equatorial plane. When we are viewing the disk from the side, we can see that the side that is spinning towards us is brighter than the side spinning away from us.

[강착원반 시뮬레이션 측면도]

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Light near a rotating black hole can travel and curves that maintain a constant distance from the black hole but trace out a spherical shell like the photon in this animation. These paths are unstable, so photon travelling on this path can easily be pushed outwards or inwards.

회전하는 블랙홀 주위를 맴도는 광자들의 운동경로는 매우 불규칙하다. 일부 광자는 안으로 빨려들고 또 어떤 광자는 사건 지평선 밖에서 튕겨나간다.


If they are pushed inwards, the photons can cross the event horizon and become lost inside the black hole. If the photons are pushed outwards, they can escape to be seen by a telescope.

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Recall the black hole's innermost circle orbit for photons, or photon sphere. Photons within the photon sphere travel and spherical orbits sometimes called the 'Ring of Fire'. Within the Ring of Fire, there was a black region called the black hole shadow, a region where light can no longer escape outside observers.

관측 가능한 가장 안쪽의 광자들의 구(Photon Sphere)를 'Ring of Fire'라 부른다. 광구 안쪽의 검은 영역을 '블랙홀 그림자(Black Hole's Shadow)'라고 하는데 사건의 지평선 안으로 빨려들어간 광자들이 더이상 관측될 수 없는 영역이다.


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The  Event Horizon Telescope is a collection of radio telescopes scattered across many locations over the earth. The event horizon telescope is observing Sagittarius A* the black hole at the center of our galaxy and eventually it will become sensitive enough to detect the black hole shadow.


전 지구에 산재한 EHT (사건의 지평선 망원경)은 거대한 전파망원경 배열이다. 우리은하내 궁수자리 A* 블랙홀 그림자의 관측이 목표다.



Computer simulation suggests that Sagittarius A* should look something like this video. This computer simulation shows an accretion disk orbiting around a black hole and shows a ring of fire around a central dark feature.

궁수자리 A*의 컴퓨터 시뮬레이션 모습이다. 블랙홀 주변을 도는 강착 원반과 광구의 모습이 보인다.


However, the image that the Event Horizon Telescope is creating will not look as sharp, since the picture will be averaged over time and there will be blurring due to light scattering off of interstellar gas and dust. This observation will be the most detailed image of the region directly outside of a Black Hole Event Horizon.

EHT로 관측될영상은 성간 물질들의 방해(전파 산란)로 인해 위사진처럼 선명하진 않을 것이다.

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10.01 - 소개: 중력 관측(Introduction: Seeing with Gravity)

10.01 - 소개: 중력 관측(Introduction: Seeing with Gravity) [커세라 강의 페이지]



Our view of black holes has been limited to the electromagnetic radiation that the material falling into the black hole gives off. But this emitted light will have to travel on curved paths in order to reach our telescopes. As a result, our views of structures near black holes will be warped.


New observations by the The Event Horizon Telescope will be able to see distortions of space caused by black holes strong gravity.

[Event Horizon Telescope  (EHT) is a large telescope array consisting of a global network of radio telescopes.]

Visible light is not the only form of electromagnetic radiation. In order to understand black holes, we have had to observe them using X-ray, ultraviolet, and radio telescopes.


Similarly, electromagnetic radiation is not the only type of radiation. When masses such as black holes move rapidly, gravitational radiation is emitted.


Modern technological advances allow scientists to see with a new kind of eyes. Once they don't see light but see the stretching and squeezing of space-time itself.

현대의 과학기술의 발전은 새로운 눈을 제공했는데, 빛을 보는것이 니라 시공간이 줄었다 늘었다 하는 모습을 관측할 수 있게 해준다.





By using gravity to probe into the heart of black holes, we can determine details that would otherwise be hidden behind the dust and gas of an accretion disk.

Gravitational waves predicted by Einstein have recently become the hot new tool to generate scientific data on the behaviors of black holes and compact objects in extreme orbits.

아인슈타인에 의해 예측되었던 중력파는 블랙홀에 관한 과학 정보를 수집하는 중요한 도구가 되었다. [중력파를 관측하여 블랙홀의 중요한 자료를 수집할 수 있게 되었다.] 아주 멀리 떨어진 곳에서 중력파를 검출 하게 됐다.

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In order to see a gravitational wave, there are a couple options: we can measure the influence of a passing wave on laser beams, or we could precisely time how the pulses of fast rotating pulsars change when a gravitational wave passes by.

중력파를 검출 하기 위한 몇가지 방법이 있는데, 중력파가 레이져 광선을 통과할 때 일으키는 미세한 변화를 검출하는 방법과 중력파가 빠르게 회전하는 펄서를 지날 때 일으키는 변화를 측정하는 방법이다.

Let's start with the simplest way the black hole's gravity effects are observations. Gravitational lensing.

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