
Last time I described some of the talks at James Hartle's 60th birthday celebration at the Newton Institute. But I also met some people at that party that I'd been wanting to talk to. There's a long story behind this, so if you don't mind, I'll start at the beginning....
A while ago, Phillip Helbig, one of the two moderators of sci.physics.research who do astrophysics, drew my attention to an interesting paper:
1) Vipul Periwal, Cosmological and astrophysical tests of quantum gravity, preprint available at astroph/9906253
The basic idea behind this is that quantum gravity effects could cause deviations from Newton's inverse square law at large distance scales, and that these deviations might explain various puzzles in astrophysics, like the "missing mass problem" and the possibly accelerating expansion of the universe.
This would be great, because it might not only help us understand these astrophysics puzzles, but also help solve the big problem with quantum gravity, namely the shortage of relevant experimental data.
But of course one needs to read the fine print before getting too excited about ideas like this!
Following the argument in Periwal's paper requires some familiarity with the renormalization group, since that's what people use to study how "constants" like the charge of the electron or Newton's gravitational constant depend on the distance scale at which you measure them  due to quantum effects. Reading the paper, I immediately became frustrated with my poor understanding of the renormalization group. It's really important, so I decided to read more about it and explain it in the simplest possible terms on sci.physics.research  since to understand stuff, I like to try to explain it.
In the process, I found this book very helpful:
1) Michael E. Peskin and Daniel V. Schroeder, An Introduction to Quantum Field Theory, AddisonWesley, Reading, Massachusetts 1995.
The books I'd originally learned quantum field theory from didn't incorporate the modern attitude towards renormalization, due to Kenneth Wilson  the idea that quantum field theory may not ultimately be true at very short distance scales, but that's okay, because if we assume it's a good approximation at pretty short distance scales, it becomes a better approximation at larger distance scales. This is especially important when you're thinking about quantum gravity, where godawful strange stuff may be happening at the Planck length. Peskin and Schroeder explain this idea quite well. For my own sketchy summary, try this:
2) John Baez, Renormalization made easy, http://math.ucr.edu/home/baez/renormalization.html
I deliberately left out as much math as possible, to concentrate on the basic intuition.
Thus fortified, I returned to Periwal's paper, and it made a bit more sense. Let me describe the main idea: how we might expect Newton's gravitational constant to change with distance.
So, suppose we have any old quantum field theory with a coupling constant G in it. In fact, G will depend on the length scale at which we measure it. But using Planck's constant and the speed of light we can translate length into 1/momentum. This allows us to think of G as a function of momentum. Roughly speaking, when you shoot particles at each other at higher momenta, they come closer together before bouncing off, so measuring a coupling constant at a higher momentum amounts to measuring at a shorter distance scale.
The equation describing how G depends on the momentum p is called the "CallanSymanzik equation". In general it looks like this:
dG  = β(G) d(ln p)But all the fun starts when we use our quantum field theory to calculate the right hand side, which is called  surprise!  the "beta function" of our theory. Typically we get something like this:
dG  = (n  d)G + aG^{2} + bG^{3} + .... d(ln p)Here n is the dimension of spacetime and d is a number called the "upper critical dimension". You see, it's fun when possible to think of our quantum field theory as defined in a spacetime of arbitrary dimension, and then specialize to the case at hand. I'll show you how work out d in a minute. It's harder to work out the numbers a, b, and so on  for this, you need to do some computations using the quantum field theory in question.
What does the CallanSymanzik equation really mean? Well, for starters let's neglect the higherorder terms and suppose that
dG(p)  = (n  d)G d(ln p)This says G is proportional to p^{nd}. There are 3 cases:
A) When n < d, our coupling constant gets smaller at higher momentum scales, and we say our theory is "superrenormalizable". Roughly, this means that at larger and larger momentum scales, our theory looks more and more like a "free field theory"  one where particles don't interact at all. This makes superrenormalizable theories easy to study by treating them as a free field theory plus a small perturbation.
B) When n > d, our coupling constant gets larger at higher momentum scales, and we say our theory is "nonrenormalizable". Such theories are hard to study using perturbative calculations in free field theory.
C) When n = d, we are right on the brink between the two cases above. We say our theory is "renormalizable", but we really have to work out the next term in the beta function to see if the coupling constant grows or shrinks with increasing momentum.
Consider the example of general relativity. We can figure out the upper critical dimension using a bit of dimensional analysis and handwaving. Let's work in units where Planck's constant and the speed of light are 1. The Lagrangian is the Ricci scalar curvature divided by 8 π G, where G is Newton's gravitational constant. We need to get something dimensionless when we integrate the Lagrangian over spacetime to get the action, since we exponentiate the action when doing path integrals in quantum field theory. Curvature has dimensions of 1/length^{2}, so when spacetime has dimension n, G must have dimensions of length^{n2}.
This means that if you are a tiny little person with a ruler X times smaller than mine, Newton's constant will seem X^{n2} times bigger to you. But measuring Newton's constant at a length scale that's X times smaller is the same as measuring it at a momentum scale that's X times bigger. We already solved the CallanSymanzik equation and saw that when we measure G at the momentum scale p, we get an answer proportional to p^{nd}. We thus conclude that d = 2.
(If you're a physicist, you might enjoy finding the holes in the above argument, and then plugging them.)
This means that quantum gravity is nonrenormalizable in 4 dimensions. Apparently gravity just keeps looking stronger and stronger at shorter and shorter distance scales. That's why quantum gravity has traditionally been regarded as hard  verging on hopeless.
However, there is a subtlety. We've been ignoring the higherorder terms in the beta function, and we really shouldn't!
This is obvious for renormalizable theories, since when n = d, the beta function looks like
dG  = aG^{2} + bG^{3} + .... d(ln p)so if we ignore the higherorder terms, we are ignoring the whole righthand side! To see the effect of these higherorder terms let's just consider the simple case where
dG  = aG^{2} d(ln p)If you solve this you get
c G =  1  ac ln pwhere c is a positive constant. What does this mean? Well, if a < 0, it's obvious even before solving the equation that G slowly decreases with increasing momentum. In this case we say our theory is "asymptotically free". For example, this is true for the strong force in the Standard Model, so in collisions at high momentum quarks and gluons act a lot like free particles. (For more on this, try "week94".)
On the other hand, if a > 0, the coupling constant G increases with increasing momentum. To make matters worse, it becomes INFINITE at a sufficiently high momentum! In this case we say our theory has a "Landau pole", and we cluck our tongues disapprovingly, because it's not a good thing. For example, this is what happens in quantum electrodynamics when we don't include the weak force. Of course, one should really consider the effect of even higherorder terms in the beta function before jumping to conclusions. However, particle physicists generally feel that among renormalizable field theories, the ones with a < 0 are good, and the ones with a > 0 are bad.
Okay, now for the really fun part. Perturbative quantum gravity in 2 dimensions is not only renormalizable (because this is the upper critical dimension), it's also asympotically free! Thus in n dimensions, we have
dG  = (n  2)G + aG^{2} + .... d(ln p)where a < 0. If we ignore the higherorder terms which I have written as "....", this implies something very interesting for quantum gravity in 4 dimensions. Suppose that at low momenta G is small. Then the righthand side is dominated by the first term, which is positive. This means that as we crank up the momentum scale, G keeps getting bigger. This is what we already saw about nonrenormalizable theories. But after a while, when G gets big, the second term starts mattering more  and it's negative. So the growth of G starts slowing!
In fact, it's easy to see that as we keep cranking up the momentum, G will approach the value for which
dG  = 0 d(ln p)We call this value an "ultraviolet stable fixed point" for the gravitational constant. Mathematically, what we've got is a flow in the space of coupling constants, and an ultraviolet stable fixed point is one that attracts nearby points as we flow in the direction of higher momenta. This particular kind of ultraviolet stable fixed point  coming from an asymptotically free theory in dimensions above its upper critical dimension  is called a "WilsonFisher fixed point".
So: perhaps quantum gravity is saved from an evergrowing Newton's constant at small distance scales by a WilsonFisher fixed point! But before we break out the champagne, note that we neglected the higherorder terms in the beta function in our last bit of reasoning. They can still screw things up. For example, if
dG  = (n  2)G + aG^{2} + bG^{3} d(ln p)and b is positive, there will not be a WilsonFisher fixed point when the dimension n gets too far above 2. Is 4 too far above 2? Nobody knows for sure. We can't really work out the beta function exactly. So, as usual in quantum gravity, things are a bit iffy.
However, Periwal cites the following paper as giving numerical evidence for a WilsonFisher fixed point in quantum gravity:
3) Herbert W. Hamber and Ruth M. Williams, Newtonian potential in quantum Regge gravity, Nucl. Phys. B435 (1995), 361397.
And he draws some startling conclusions from the existence of this fixed point. He says it should have consequences for the missing mass problem and the value of the cosmological constant! However, I found it hard to follow his reasoning, so I decided to track down some of the references  starting with the above paper.
Now, Ruth Williams works at Cambridge University, so I was not surprised to find her at Hartle's party. She was busy talking to John Barrett, who also does quantum gravity, up at Nottingham University. I arranged to stop by her office, get a copy of her paper, and have her explain it to me. I also arranged to visit John in Nottingham and have him explain his work with Louis Crane on Lorentzian spin foam models  but more about that next week!
Anyway, here's how the HamberWilliams paper goes, very roughly. They simulate quantum gravity by chopping up a 4dimensional torus into 16 x 16 x 16 x 16 hypercubes, chopping each hypercube into 24 4simplices in the obvious way, and then doing a Monte Carlo calculation of the path integral using the Regge calculus, which is a discretized version of general relativity suited to triangulated manifolds (see "week119" for details). Their goal was to work out how Newton's constant varies with distance. They did it by calculating correlations between Wilson loops that wrap around the torus. They explain how you can deduce Newton's constant from this information, but I don't have the energy to describe that here. Anyway, they claim that Newton's constant varies with distance as one would expect if there was a WilsonFisher fixed point!
(It's actually more complicated that this because besides Newton's constant, there is also another coupling constant in their theory: the cosmological constant. And of course this is very important for potential applications to astrophysics.)
Unfortunately, I'm still mystified about a large number of things. Let me just mention two. First, Hamber and Williams consider values of G which are greater than the WilsonFisher fixed point. Since this is an ultraviolet stable fixed point, such values of G flow down to the fixed point as we crank up the momentum scale. Or in other words, in this regime Newton's constant gets bigger with increasing distances. At least to my naive brain, this sounds nice for explaining the missing mass problem. But the funny thing is, this regime is utterly different from the regime where G is close to zero  namely, less than the WilsonFisher fixed point. I thought all the usual perturbative quantum gravity calculations were based on the assumption that at macroscopic distance scales G is small, and flows up to the fixed point as we crank up the momentum scale! Are these folks claiming this picture is completely wrong? I'm confused.
Another puzzle is that Periwal thinks Newton's constant will start to grow at distance scales roughly comparable to the radius of the universe (or more precisely, the Hubble length). But it looks like Hamber and Williams say their formula for G as a function of momentum holds at short distance scales.
I guess I need to read more stuff, starting perhaps with Weinberg's old paper on quantum gravity and the renormalization group:
4) Steven Weinberg, Ultraviolet divergences in quantum theories of gravitation, in General Relativity: an Einstein Centenary Survey, eds. Stephen Hawking and Werner Israel, Cambridge U. Press, Cambridge (1979).
and then perhaps turning to his paper on the cosmological constant:
5) Steven Weinberg, The cosmological constant problem, Rev. Mod. Phys. 61 (1989), 1.
and some books on the renormalization group and quantum gravity:
6) Claude Itzykson and JeanMichel Drouffe, Statistical Field Theory, 2 volumes, Cambridge U. Press, 1989.
7) Jean ZinnJustin, Quantum Field Theory and Critical Phenomena, Oxford U. Press, Oxford, 1993.
8) Jan Ambjorn, Bergfinnur Durhuus, and Thordur Jonsson, Quantum Geometry: A Statistical Field Theory Approach, Cambridge U. Press, Cambridge, 1997.
I should also think more about this recent paper, which claims to find a phase transition in a toy model of quantum gravity where one does the path integral over a special class of metrics  namely those with 2 Killing vector fields.
9) Viqar Husain and Sebastian Jaimungal, Phase transition in quantum gravity, preprint available as grqc/9908056.
But if anyone can help me clear up these issues, please let me know!
Okay, enough of that. Another person I met at the party was Roger Penrose! Later I visited him in Oxford. Though recently retired, he still holds monthly meetings at his house in the country, attended by a bunch of young mathematicians and physicists. At the one I went to, the discussion centered around Penrose's forthcoming book. The goal of this book is to explain modern physics to people who know only a little math, but are willing to learn more. A nice thing about it is that it treats various modern physics fads without the uncritical adulation that mars many popularizations. In particular, when I visited, he was busy writing a chapter on inflationary cosmology, so he talked about a bunch of problems with that theory, and cosmology in general.
I've never been sold on inflation, since it relies on fairly speculative aspects of grand unified theories (or GUTs), so most of these problems merely amused me. Theorists take a certain wicked glee in seeing someone else's theory in trouble. However, one of these problems concerned the Standard Model, and this hit closer to home. Penrose made the standard observation that the most distant visible galaxies in opposite directions have not had time to exchange information  at least not since the time of recombination, when the initial hot fireball cooled down enough to become transparent. But if the symmetry between the electromagnetic and weak forces is spontaneously broken only when the Higgs field cools down enough to line up, as the Standard Model suggests, this raises the danger that the Higgs field could wind up pointing in different directions in different patches of the visible universe!  since these different "domains" would not yet have had time to expand to the point where a single one fills the whole visible universe. But we don't see such domains  or more precisely, we don't see the "domain walls" one would expect at their boundaries.
Of course, inflation is an attempt to deal with similar problems, but inflation is posited to happen at GUT scale energies, too soon (it seems) to solve this problem, which happens when things cool down to the point where the electroweak symmetry breaks.
Again, if anyone knows anything about this, I'd love to hear about it.
