**Introduction**

In 1994 Stephen W. Hawking and Roger Penrose gave a series of public lectures on general relativity at the Isaac Newton Institute for Mathematical Sciences at the University of Cambridge. From these lectures, published this year by Princeton University Press as The Nature of Space and Time, Scientific American has culled excerpts that serve to compare and contrast the perspectives of the two scientists. Although they share a common heritage in physics-Penrose served on Hawking's Ph.D. thesis committee at Cambridge-the lecturers differ in their vision of quantum mechanics and its impact on the evolution of the universe. In particular, Hawking and Penrose disagree on what happens to the information stored in a black hole and on why the beginning of the universe differs from the end.

One of Hawking's major discoveries, made in 1973, was that quantum effects will cause black holes to emit particles. The black hole will evaporate in the process, so that ultimately perhaps nothing of the original mass will be left. But during their formation, black holes swallow a lot of data-the types, properties and configurations of the particles that fall in. Although quantum theory requires that such information must be conserved, what finally happens to it remains a topic of contentious debate. Hawking and Penrose both believe that when a black hole radiates, it loses the information it held. But Hawking insists that the loss is irretrievable, whereas Penrose argues that the loss is balanced by spontaneous measurements of quantum states that introduce information back into the system.

Both scientists agree that a future quantum theory of gravity is needed to describe nature. But they differ in their view of some aspects of this theory. Penrose thinks that even though the fundamental forces of particle physics are symmetric in time-unchanged if time is reversed-quantum gravity will violate time symmetry. The time asymmetry will then explain why in the beginning the universe was so uniform, as evinced by the microwave background radiation left over from the big bang, whereas the end of the universe must be messy.

Penrose attempts to encapsulate this time asymmetry in his Weyl curvature hypothesis. Space-time, as Albert Einstein discovered, is curved by the presence of matter. But space-time can also have some intrinsic bending, a quantity designated by the Weyl curvature. Gravitational waves and black holes, for example, allow space-time to curve even in regions that are empty. In the early universe the Weyl curvature was probably zero, but in a dying universe the large number of black holes, Penrose argues, will give rise to a high Weyl curvature. This property will distinguish the end of the universe from the beginning.

Hawking agrees that the big bang and the final "big crunch" will be different, but he does not subscribe to a time asymmetry in the laws of nature. The underlying reason for the difference, he thinks, is the way in which the universe's evolution is programmed. He postulates a kind of democracy, stating that no point in the universe can be special; therefore, the universe cannot have a boundary. This no-boundary proposal, Hawking claims, explains the uniformity in the microwave background radiation.

The physicists diverge, ultimately, in their interpretation of
quantum mechanics. Hawking believes that all a theory has to do
is provide predictions that agree with data. Penrose thinks that
simply comparing predictions with experiments is not enough to
explain reality. He points out that quantum theory requires wave
functions to be "superposed," a concept that can lead
to absurdities. The scientists thus pick up the threads of the
famous debates
between Einstein and Niels Bohr on the bizarre implications
of quantum theory. -*The Editors*

Copyright ©1996 by Princeton University Press. From the book
entitled *The Nature of Space and Time *by Stephen Hawking
and Roger Penrose, published by Princeton University Press.
Printed by permission.

**Stephen Hawking on quantum black holes****:**

The quantum theory of black holes...seems to lead to a new level of unpredictability in physics over and above the usual uncertainty associated with quantum mechanics. This is because black holes appear to have intrinsic entropy and to lose information from our region of the universe. I should say that these claims are controversial: many people working on quantum gravity, including almost all those who entered it from particle physics, would instinctively reject the idea that information about the quantum state of a system could be lost. However, they have had very little success in showing how information can get out of a black hole. Eventually I believe they will be forced to accept my suggestion that it is lost, just as they were forced to agree that black holes radiate, which went against all their preconceptions...

The fact that gravity is attractive means that it will tend to
draw the matter in the universe together to form objects like
stars and galaxies. These can support themselves for a time
against further contraction by thermal pressure, in the case of
stars, or by rotation and internal motions, in the case of
galaxies. However, eventually the heat or the angular momentum
will be carried away and the object will begin to shrink. If the
mass is less than about one and a half times that of the Sun, the
contraction can be stopped by the *degeneracy pressure***
**of electrons
or neutrons. The object will settle down to be a white
dwarf or a neutron
star, respectively. However, if the mass is greater than this
limit there is nothing that can hold it up and stop it continuing
to contract. Once it has shrunk to a certain critical size the
gravitational field at its surface will be so strong that the

Thus there must be a region of space-time from which it is not
possible to escape to infinity. This region is said to be a black
hole. Its boundary is called the event horizon and is a *null surface***
**formed by the light rays that just fail to get away to
infinity.... Computer
animations help clarify some of there peculiar phenomena

[A] large amount of information is lost when a body collapses
to form a black hole. The collapsing body is described by a very
large number of parameters. There are the types of matter and the
*multipole moments***
**of the mass distribution. Yet the black hole that forms
is completely independent of the type of matter and rapidly loses
all the multipole moments except the first two: the monopole
moment, which is the mass, and the dipole moment, which is the
angular momentum.

This loss of information didn't really matter in the classical theory. One could say that all the information about the collapsing body was still inside the black hole. It would be very difficult for an observer outside the black hole to determine what the collapsing body was like. However, in the classical theory it was still possible in principle. The observer would never actually lose sight of the collapsing body. Instead it would appear to slow down and get very dim as it approached the event horizon. But the observer could still see what it was made of and how the mass was distributed.

However, quantum theory changed all this. First, the collapsing body would send out only a limited number of photons before it crossed the event horizon. They would be quite insufficient to carry all the information about the collapsing body. This means that in quantum theory there's no way an outside observer can measure the state of the collapsed body. One might not think that this mattered too much, because the information would still be inside the black hole even if one couldn't measure it from the outside. But this is where the second effect of quantum theory on black holes comes in....

[Quantum] theory will cause black holes to radiate and lose mass. It seems that they will eventually disappear completely, taking with them the information inside them. I will give arguments that this information really is lost and doesn't come back in some form. As I will show, this loss of information would introduce a new level of uncertainty into physics over and above the usual uncertainty associated with quantum theory. Unfortunately, unlike Heisenberg's uncertainty principle, this extra level will be rather difficult to confirm experimentally in the case of black holes.

**Roger Penrose on quantum theory and
space-time****:**

The great physical theories of the 20th century have been quantum theory, special relativity, general relativity and quantum field theory. These theories are not independent of each other: general relativity was built on special relativity, and quantum field theory has special relativity and quantum theory as inputs.

It has been said that quantum field theory is the most
accurate physical theory ever, being accurate to about one part
in about 10^{11}. However, I would like to point out that
general relativity has, in a certain clear sense, now been tested
to be correct to one part in 10^{14} (and this accuracy
has apparently been limited merely by the accuracy of clocks on
Earth). I am speaking of the Hulse-Taylor
binary *pulsar*** **PSR 1913+16, a pair
of neutron stars orbiting each other, one of which is a pulsar. General
relativity predicts that this orbit will slowly decay (and the
period shorten) because energy is lost through the emission of
gravitational waves. This has indeed been observed, and the
entire description of the motion...agrees with general relativity
(which I am taking to include Newtonian theory) to the remarkable
accuracy, noted above, over an accumulated period of 20 years.
The discoverers of this system have now rightly been awarded Nobel
Prizes for their work. The quantum theorists have always
claimed that because of the accuracy of their theory, it should
be general relativity that is changed to fit their mold, but I
think now that it is quantum field theory that has some catching
up to do.

Although these four theories have been remarkably successful,
they are not without their problems....General relativity
predicts the existence of space-time *singularities*** .
**In quantum theory there is the "measurement problem"-I
shall describe this later. It may be taken that the solution to
the various problems of these theories lies in the fact that they
are incomplete on their own. For example, it is anticipated by
many that quantum field theory might "smear" out the
singularities of general relativity in some way....

I should now like to talk about information loss in black holes, which I claim is relevant to this last issue. I agree with nearly all that Stephen had to say on this. But while Stephen regards the information loss due to black holes as an extra uncertainty in physics, above and beyond the uncertainty from quantum theory, I regard it as a "complementary" uncertainty.... It is possible that a little bit of information escapes at the moment of the black hole evaporation...but this tiny information gain will be much smaller than the information loss in the collapse (in what I regard as any reasonable picture of the hole's final disappearance).

If we enclose the system in a vast box, as a thought
experiment, we can consider the ** phase-space**
evolution of matter inside the box. In the region of

[Let] us consider the *Schroedinger's cat***
**thought experiment. It describes the plight of a cat in a
box, where (let us say) a photon is emitted which encounters a
half-silvered mirror, and the transmitted part of the photon's
wave function encounters a detector which, if it detects the
photon, automatically fires a gun, killing the cat. If it fails
to detect the photon, then the cat is alive and well. (I know
Stephen does not approve of mistreating
cats, even in a thought experiment!) The wave function of the
system is a superposition of these two possibilities....But why
does our perception not allow us to perceive macroscopic
superpositions, of states such as these, and not just the
macroscopic alternatives "cat is dead" and "cat is
alive"?...

I am suggesting that something goes wrong with superpositions
of the alternative space-time geometries that would occur when
general relativity begins to become involved. Perhaps a
superposition of two different geometries is unstable and decays
into one of the two alternatives. For example, the geometries
might be the space-times of a live cat, or a dead one. I call
this decay into one **or **the other alternative objective
reduction, which I like as a name because it has an appropriately
nice acronym (OR). How does the Planck length 10^{-33}
centimeter relate to this? Nature's criterion for determining
when two geometries are significantly different would depend upon
the *Planck scale*** ,
**and this fixes the timescale in which the reduction into
different alternatives occurs.

I will end this lecture on a topic on which Roger and I have
very different views-the arrow of time.** **There is a very
clear distinction between the forward and the backward directions
of time in our region of the universe. One only has to watch a
film being run backward to see the difference. Instead of cups
falling off tables and getting broken, they would mend themselves
and jump back on the table. If only real life were like that.

The local laws that physical fields obey are time symmetric,
or more precisely, *CPT (charge-parity-time)
invariant*** . **Thus, the observed
difference between the past and the future must come from the
boundary conditions of the universe. Let us take it that the
universe is spatially closed and that it expands to a maximum
size and collapses again. As Roger has emphasized, the universe
will be very different at the two ends of this history. At what
we call the beginning of the universe, it seems to have been very
smooth and regular. However, when it collapses again, we expect
it to be very disordered and irregular. Because there are so many
more disordered configurations than ordered ones, this means that
the initial conditions would have had to be chosen incredibly
precisely.

It seems, therefore, that there must be different boundary
conditions at the two ends of time. Roger's proposal is that the *Weyl tensor***
**should vanish at one end of time but not the other. The
Weyl tensor is that part of the curvature of space-time that is
not locally determined by the matter through the Einstein
equations. It would have been small in the smooth, ordered early
stages but large in the collapsing universe. Thus, this proposal
would distinguish the two ends of time and so might explain the
arrow of time.

I think Roger's proposal is Weyl in more than one sense of the word. First, it is not CPT invariant. Roger sees this as a virtue, but I feel one should hang on to symmetries unless there are compelling reasons to give them up. Second, if the Weyl tensor had been exactly zero in the early universe, it would have been exactly homogeneous and isotropic and would have remained so for all time. Roger's Weyl hypothesis could not explain the fluctuations in the background nor the perturbations that give rise to galaxies and bodies like ourselves.

Despite all this, I think Roger has put his finger on an
important difference between the two ends of time. But the fact
that the Weyl tensor was small at one end should not be imposed
as an ad hoc boundary condition but should be deduced from a more
fundamental principle, the *no-boundary proposal**....*

How can the two ends of time be different? Why should
perturbations be small at one end but not the other? The reason
is there are two possible complex solutions of the field
equations** ....** Obviously, one solution corresponds
to one end of time and the other to the other

From what I understand of Stephen's position, I don't think
that our disagreement is very great on this point [** the Weyl curvature
hypothesis**].

Maybe the no-boundary proposal of [James B.] Hartle and
Hawking is a good candidate for the structure of the *initial *state.
However, it seems to me that we need something very different to
cope with the *final* state. In particular, a theory that
explains the structure of singularities would have to violate [CPT and other symmetries] in
order that something of the nature of the Weyl curvature
hypothesis can arise. This failure of time-symmetry might be
quite subtle; it would have to be implicit in the rules of that
theory which goes beyond quantum mechanics.

**Hawking**** on physics and
reality:**

These lectures have shown very clearly the difference between
Roger and me. He's a Platonist and I'm a positivist. He's worried
that Schroedinger's cat is in a quantum state, where it is half
alive and half dead. He feels that can't correspond to reality.
But that doesn't bother me. I don't demand that a theory
correspond to reality because I don't know what it is. Reality is
not a quality you can test with litmus paper. All I'm concerned
with is that the theory should predict the results of
measurements. Quantum theory does this very successfully*....*

Roger feels that** ...**the collapse of the wave
function introduces CPT violation into physics. He sees such
violations at work in at least two situations: cosmology and
black holes. I agree that we may introduce time asymmetry in the
way we ask questions about observations. But I totally reject the
idea that there is some physical process that corresponds to the
reduction of the wave function or that this has anything to do
with quantum gravity or consciousness.
That sounds like magic to me, not science.

**Penrose**** on physics and
reality:**

Quantum mechanics has only been around for 75 years. This is not very long if one compares it, for example, with Newton's theory of gravity. Therefore it wouldn't surprise me if quantum mechanics will have to be modified for very macroscopic objects.

At the beginning of this debate, Stephen said that he thinks that he is a positivist, whereas I am a Platonist. I am happy with him being a positivist, but I think that the crucial point here is, rather, that I am a realist. Also, if one compares this debate with the famous debate of Bohr and Einstein, some 70 years ago, I should think that Stephen plays the role of Bohr, whereas I play Einstein's role! For Einstein argued that there should exist something like a real world, not necessarily represented by a wave function, whereas Bohr stressed that the wave function doesn't describe a "real" microworld but only "knowledge" useful for making predictions.

Bohr was perceived to have won the argument. In fact, according to the recent biography of Einstein by [Abraham] Pais, Einstein might as well have gone fishing from 1925 onward. Indeed, it is true that he didn't make many big advances, even though his penetrating criticisms were very useful. I believe that the reason why Einstein didn't continue to make big advances in quantum theory was that a crucial ingredient was missing from quantum theory. This missing ingredient was Stephen's discovery, 50 years later, of black hole radiation. It is this information loss, connected with black hole radiation, which provides the new twist.

*The Editors acknowledge the assistance of **Gary
T. Horowitz** of the University of California at Santa
Barbara.*