Math explains black hole light bending visual trick
Math explains how light curving around black holes can reveal multiple images of the same galaxies to observers, according to a new study.
A new study pins down a phenomenon that allows light to curve around black holes to present an observer with multiple views of the same background galaxy.
In the vicinity of a black hole, space curves so much that light rays are deflected, and very nearby light can be deflected so much that it travels several times around the black hole. Therefore, when we observe a distant galaxy (or some other celestial body) in the background, we may be lucky to see the same image of the galaxy multiple times, albeit more and more distorted.
“There is something fantastically beautiful in now understanding why the images repeat themselves in such an elegant way.”
The mechanism is shown on the figure below: A distant galaxy shines in all directions—some of its light comes close to the black hole and is lightly deflected; some light comes even closer and circumvolves the hole a single time before escaping down to us, and so on. Looking near the black hole, we see more and more versions of the same galaxy, the closer to the edge of the hole we are looking.
How much closer to the black hole do you have to look from one image to see the next image? The result has been known for over 40 years, and is some 500 times (for the math aficionados, it is more accurately the “exponential function of two pi”, written e2π).
Calculating this is so complicated that, until recently, we had not yet developed a mathematical and physical intuition as to why it happens to be this exact factor. But using some clever, mathematical tricks, master’s student Albert Sneppen from the Cosmic Dawn Center—a basic research center under both the Niels Bohr Institute and DTU Space at the University of Copenhagen—has now succeeded in proving why.
“There is something fantastically beautiful in now understanding why the images repeat themselves in such an elegant way. On top of that, it provides new opportunities to test our understanding of gravity and black holes,” Sneppen says.
Proving something mathematically is not only satisfying in itself; indeed, it brings us closer to an understanding of this marvelous phenomenon. The factor “500” follows directly from how black holes and gravity work, so the repetitions of the images now become a way to examine and test gravity.
As a completely new feature, Sneppen’s method can also be generalized to apply not only to “trivial” black holes, but also to black holes that rotate . Which, in fact, they all do.
“It turns out that when the it rotates really fast, you no longer have to get closer to the black hole by a factor 500, but significantly less. In fact, each image is now only 50, or 5, or even down to just 2 times closer to the edge of the black hole,” explains Sneppen.
Having to look 500 times closer to the black hole for each new image, means that the images are quickly “squeezed” into one annular image. In practice, the many images will be difficult to observe. But when black holes rotate, there is more room for the “extra” images, so we can hope to confirm the theory observationally in a not-too-distant future. In this way, we can learn about not just black holes, but also the galaxies behind them.
The travel time of the light increases, the more times it has to go around the black hole, so the images become increasingly “delayed.” If, for example, a star explodes as a supernova in a background galaxy, one would be able to see this explosion again and again.
The research appears in Scientific Reports .
Source: University of Copenhagen
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