Nautilus Members enjoy an ad-free experience. or Join now .

Why Stephen Hawking’s Black Hole Puzzle Keeps Puzzling

The renowned British physicist, who died at 76, left behind a riddle that could eventually lead his successors to the theory of quantum gravity.

Article Lead Image

The renowned British physicist Stephen Hawking, who died on March 14 at 76, was something of a betting man, regularly entering into friendly wagers with his colleagues over key questions in theoretical physics. “I sensed when Stephen and I first met that he would enjoy being treated irreverently,” wrote John Preskill, a physicist at the California Institute of Technology, earlier today on Twitter. “So in the middle of a scientific discussion I could interject, ‘What makes you so sure of that, Mr. Know-It-All?’ knowing that Stephen would respond with his eyes twinkling: ‘Wanna bet?’”

And bet they did. In 1991, Hawking and Kip Thorne bet Preskill that information that falls into a black hole gets destroyed and can never be retrieved. Called the black hole information paradox, this prospect follows from Hawking’s landmark 1974 discovery about black holes—regions of inescapable gravity, where space-time curves steeply toward a central point known as the singularity. Hawking had shown that black holes are not truly black. Quantum uncertainty causes them to radiate a small amount of heat, dubbed “Hawking radiation.” They lose mass in the process and ultimately evaporate away. This evaporation leads to a paradox: Anything that falls into a black hole will seemingly be lost forever, violating “unitarity”—a central principle of quantum mechanics that says the present always preserves information about the past.

Nautilus Members enjoy an ad-free experience. Log in or Join now .

Hawking and Thorne argued that the radiation emitted by a black hole would be too hopelessly scrambled to retrieve any useful information about what fell into it, even in principle. Preskill bet that information somehow escapes black holes, even though physicists would presumably need a complete theory of quantum gravity to understand the mechanism behind how this could happen.

Physicists thought they resolved the paradox in 2004 with the notion of black hole complementarity. According to this proposal, information that crosses the event horizon of a black hole both reflects back out and passes inside, never to escape. Because no single observer can ever be both inside and outside the black hole’s horizon, no one can witness both situations simultaneously, and no contradiction arises. The argument was sufficient to convince Hawking to concede the bet. During a July 2004 talk in Dublin, Ireland, he presented Preskill with the eighth edition of Total Baseball: The Ultimate Baseball Encyclopedia, “from which information can be retrieved at will.”

Nautilus Members enjoy an ad-free experience. Log in or Join now .
NASA/Goddard Space Flight Center/CI Lab

Thorne, however refused to concede, and it seems he was right to do so. In 2012, a new twist on the paradox emerged. Nobody had explained precisely how information would get out of a black hole, and that lack of a specific mechanism inspired Joseph Polchinski and three colleagues to revisit the problem. Conventional wisdom had long held that once someone passed the event horizon, they would slowly be pulled apart by the extreme gravity as they fell toward the singularity. Polchinski and his co-authors argued that instead, in-falling observers would encounter a literal wall of fire at the event horizon, burning up before ever getting near the singularity.

At the heart of the firewall puzzle lies a conflict between three fundamental postulates. The first is the equivalence principle of Albert Einstein’s general theory of relativity: Because there’s no difference between acceleration due to gravity and the acceleration of a rocket, an astronaut named Alice shouldn’t feel anything amiss as she crosses a black hole horizon. The second is unitarity, which implies that information cannot be destroyed. Lastly, there’s locality, which holds that events happening at a particular point in space can only influence nearby points. This means that the laws of physics should work as expected far away from a black hole, even if they break down at some point within the black hole—either at the singularity or at the event horizon.

To resolve the paradox, one of the three postulates must be sacrificed, and nobody can agree on which one should get the axe. The simplest solution is to have the equivalence principle break down at the event horizon, thereby giving rise to a firewall. But several other possible solutions have been proposed in the ensuing years.

Nautilus Members enjoy an ad-free experience. Log in or Join now .

For instance, a few years before the firewalls paper, Samir Mathur, a string theorist at Ohio State University, raised similar issues with his notion of black hole fuzzballs. Fuzzballs aren’t empty pits, like traditional black holes. They are packed full of strings (the kind from string theory) and have a surface like a star or planet. They also emit heat in the form of radiation. The spectrum of that radiation, Mathur found, exactly matches the prediction for Hawking radiation. His “fuzzball conjecture” resolves the paradox by declaring it to be an illusion. How can information be lost beyond the event horizon if there is no event horizon?

Hawking himself weighed in on the firewall debate along similar lines by way of a two-page, equation-free paper posted to the scientific preprint site in late January 2014—a summation of informal remarks he’d made via Skype for a small conference the previous spring. He proposed a rethinking of the event horizon. Instead of a definite line in the sky from which nothing could escape, he suggested there could be an “apparent horizon.” Information is only temporarily confined behind that horizon. The information eventually escapes, but in such a scrambled form that it can never be interpreted. He likened the task to weather forecasting: “One can’t predict the weather more than a few days in advance.”

Nautilus Members enjoy an ad-free experience. Log in or Join now .

In 2013, Leonard Susskind and Juan Maldacena, theoretical physicists at Stanford University and the Institute for Advanced Studies, respectively, made a radical attempt to preserve locality that they dubbed “ER = EPR.” According to this idea, maybe what we think are faraway points in space-time aren’t that far away after all. Perhaps entanglement creates invisible microscopic wormholes connecting seemingly distant points. Shaped a bit like an octopus, such a wormhole would link the interior of the black hole directly to the Hawking radiation, so the particles still inside the hole would be directly connected to particles that escaped long ago, avoiding the need for information to pass through the event horizon.

Physicists have yet to reach a consensus on any one of these proposed solutions. It’s a tribute to Hawking’s unique genius that they continue to argue about the black hole information paradox so many decades after his work first suggested it.

Nautilus Members enjoy an ad-free experience. Log in or Join now .

Lead image: The physicist Stephen Hawking in 1979 in Princeton, New Jersey. Credit: Santi Visalli/Getty Images

close-icon Enjoy unlimited Nautilus articles, ad-free, for less than $5/month. Join now

! There is not an active subscription associated with that email address.

Join to continue reading.

You’ve read your 2 free articles this month. Access unlimited ad-free stories, including this one, by becoming a Nautilus member.

! There is not an active subscription associated with that email address.

This is your last free article.

Don’t limit your curiosity. Access unlimited ad-free stories like this one, and support independent journalism, by becoming a Nautilus member.