# Black Holes Gain new Powers When They Spin Fast Enough

General relativity is a profoundly complex mathematical theory, but its description of black holes is amazingly simple. A stable black hole can be described by just three properties: its mass, its electric charge, and its rotation or spin. Since black holes aren’t likely to have much charge, it really takes just two properties. If you know a black hole’s mass and spin, you know all there is to know about the black hole.

This property is often summarized by the no-hair theorem. Specifically, the theorem asserts that once matter falls into a black hole, the only characteristic that remains is mass. You could make a black hole out of a Sun’s worth of hydrogen, chairs, or those old copies of National Geographic from Grandma’s attic, and there would be no difference. Mass is mass as far as general relativity is concerned. In every case the event horizon of a black hole is perfectly smooth, with no extra features. As Jacob Bekenstein said, black holes have no hair.

But with all its predictive power, general relativity has a problem with quantum theory. This is particularly true with black holes. If the no-hair theorem is correct, the information held within an object is destroyed when it crosses the event horizon. Quantum theory says that information can never be destroyed. So the valid theory of gravity is contradicted by the valid theory of the quanta. This leads to problems such as the firewall paradox, which can’t decide whether an event horizon should be hot or cold.

Several theories have been proposed to solve this contradiction, often involving extensions to relativity. But the difference between standard relativity and these modified theories can only be seen in extreme situations, making them difficult to study observationally. But a new paper in Physical Review Letters shows how they might be studied through the spin of a black hole.

Many modified relativity theories have an extra parameter not seen in the standard theory. Known as a massless scalar field, it allows Einstein’s model to connect with quantum theory in a way that isn’t contradictory. In this new work, the team looked at how such a scalar field connects to the rotation of a black hole. They found that at low spins, a modified black hole is indistinguishable from the standard model, but at high rotations the scalar field allows a black hole to have extra features. In other words, in these alternative models, rapidly rotating black holes can have hair.

The hairy aspects of rotating black holes would only be seen near the event horizon itself, but they would also affect merging black holes. As the authors point out, future gravitational wave observatories should be able to use rapidly rotating black holes to determine whether an alternative to general relativity is valid.

Einstein’s theory of general relativity has passed every observational challenge so far, but it will likely break down in the most extreme environments of the universe. Studies such as this show how we might be able to discover the theory that comes next.

Reference: Alexandru Dima, et al. “Spin-Induced Black Hole Spontaneous Scalarization.” Physical Review Letters 125.23 (2020): 231101.

## 2 Replies to “Black Holes Gain new Powers When They Spin Fast Enough”

1. It’s astonishing how truly exotic the Universe can be.

Notably current observations are perfectly compatible with hairless black holes, as the paper says and refer to the Ligo observations. But there is also the exceptional super massive black hole pair of the blazar galaxy OJ287 that woulddn’t keep predicted timing if “hairs” would increase gravitational wave energy loss [“Supermassive Black Hole Orbits an Even More Massive Black Hole, Crashing Through its Accretion Disk Every 12 Years” @ Universe Today].

“In short, the OJ 287 system supports the idea that black hole surfaces are symmetrical along their rotational axes. “It is important to black hole scientists that we prove or disprove the no-hair theorem,” said Mauri Valtonen, an astrophysicist from the University of Turku and a coauthor on the paper. “Without it, we cannot trust that black holes as envisaged by Hawking and others exist at all.””

Speaking of Hawking’s black hole physics, the coupling between quantum fields and gravity gives rise to Hawking radiation and gives the black hole a thermodynamic radiation temperature and so an entropy that is correlated with its surface. That would imply that state information is correlated with fields within a Planck distance from the black hole, where the field radiation emerges.

And in any case, I think this is a bit overstated: “If the no-hair theorem is correct, the information held within an object is destroyed when it crosses the event horizon. Quantum theory says that information can never be destroyed.” The no-hair theorem more precisely states that matter and radiation information – really, likelihoods of quantum field physics (of which gravity can be an example, for all we know) – is directly inaccessible for observers outside the event horizon. It is – somewhat ironically – precisely since Hawking radiation makes a black hole evaporate by radiating energy that an information problem appears. If the black hole has evaporated, where did the information go?!

One solution offered up by more quantum field physics is that of a firewall [“Black Holes: Complementarity or Firewalls?”, arXiv:1207.3123v4].

“We argue that the following three statements cannot all be true: (i) Hawking radiation is in a pure state, (ii) the information carried by the radiation is emitted from the region near the horizon, with low energy effective field theory valid beyond some microscopic distance from the horizon, and (iii) the infalling observer encounters nothing unusual at the horizon. Perhaps the most conservative resolution is that the infalling observer burns up at the horizon.”

I.e. to avoid quantum cloning, which is forbidden “[the] application of postulates 1 and 2 has thus led to the conclusion that the infalling observer will encounter high-energy modes.”

But YQMMV [Your Quantum Model May Vary].