Finally, Mathematical evidence for stability of black hole

Now there is mathematical proof that black holes are stable.

The mathematician Roy Kerr solved the equations of Einstein in 1963 and came up with a description of the spacetime outside of what is now known as a revolving black hole. It would take a few more years for the phrase to be coined.

Researchers have attempted to demonstrate the stability of these supposed Kerr black holes in the nearly six decades since his accomplishment.


That means that if I start with something that resembles a Kerr black hole and gives it a little bump—by, say, firing some gravitational waves at it—According to mathematician Jérémie Szeftel of the Sorbonne University, "what you anticipate, in the distant future, is that all will simmer down, and it will yet again look remarkably like a Kerr solution."



Similar praise was offered by former Harvard University professor Shing-Tung Yau, who had just joined the faculty at Tsinghua University.

He referred to the result as "the first important discovery" from the early 1990s, this area of generic relativity.

It's a challenging problem, he remarked. However, he emphasized that peer assessment of the new manuscript has not yet taken place. However, he praised the published report from 2021 as "comprehensive and intriguing."

According to Giorgi, since the bulk of precise approaches to Einstein's equations, one explanation for the subject of stability has been under discussion for so long, like the one discovered by Kerr, is stationary.

These formulas pertain to black holes that are static and unchanging; the black holes we observe in nature are not like that. Researchers must submit black holes to little disruptions to gauge their stability and then watch what happens to the answers that define these objects over time.

Consider sound waves striking a wineglass as an illustration. Almost often, the glass is somewhat shaken by the waves before the situation calms down. However, the glass might break if someone sings at a volume and pitch that exactly matches the object's resonance frequency.

Giorgi, Klainerman, and Szeftel questioned whether a black hole encountering gravitational waves might result in a resonance-like phenomenon.

They weighed several potential scenarios. For example, a gravitational wave could penetrate a Kerr black hole inside after crossing its event horizon. Even if the black hole's mass and rotation slightly changed, Kerr's equations would still describe it as a black hole.