*(A somewhat more technical post follows.)*

JT gravity is a model of two dimensional gravity that goes back many decades. But there’s not much going on in 2D (or (1+1) dimensions, one space and one time), I hear you cry! Well, nevertheless this turns out to be a very useful arena for studying very important quantum key properties of black holes in more realistic dimensions. Let me take a step back to unpack that.

There is a long tradition (which you might know about) of studying models of black holes in string/M-theory, in different limits and approaches, each with their own advantages and disadvantages. The simplest models are often too simple to capture some of the important features of black holes, and some models get nicely at certain aspects while having little to say about others. And of course, some of the more realistic (but still simple) black hole models are still too complicated to be directly solvable in order to reliably explore phenomena of interest.

I’d say that a certain class of models that has been discussed a lot recently has something new to offer. The prototype is something called the SYK model (Sachdev-Ye-Kitaev). It’s an even more crazy sounding starting point than 2D gravity, as it is a 1D model. There’s no space at all, just time: It is a model in (0+1) dimensions, if you like. It’s a special model of quantum mechanics, actually a bunch of \(\tilde N\) fermions (where \(\tilde N\) is large), with certain random couplings between them. It was noticed that this model, at temperature \(T\), as a simple thermal with quantum chaos, scrambles quantum information at a particular rate (measured by the “Lyapunov exponent” \(\lambda_L\)) that was associated with the scrambling rate of black holes: \(\lambda_L=2\pi k_B T/\hbar\). So it became of interest to study it as a simple, solvable model of this sort of behaviour. (Kitaev made a convincing case in a series of talks at the KITP back in 2015 that if you find a model with black-hole-like scrambling, it has a secret dual gravitational character to it, in a sense we’ve discussed here on the blog before. – I recommend looking at the talks (here and here), and also a nice paper of Maldacena, Shenker, and Stanford (also from Spring 2015) that discusses the gravitationally-motivated bounds on chaos that the SYK model saturates.).

Well, I heard people mention the SYK model increasingly over 2015 but I was thinking about too many other things (and was mostly dealing with being mostly sleep-deprived as a new dad), and so did not really pay much attention. *Bandwidth issues*, we’d say these days. I was happy to declare “we’ve got some of our best people on it”, and continued chipping away on other things where I could. Then in December 2017 I found myself sitting next to David Gross on a flight to the East coast (long story I forgot to blog about), and he mentioned that he’d been really excited by the SYK model and maybe I should have a look, since there’s a lot there that I’d probably like. And *still* some time went by without me clearing up bandwidth to look at any of it.

Catch up began in the Fall of last year (2019), but only after similarly missing following what was going on in a related area: JT gravity. One way of thinking about how JT gravity enters the story is to simply state that it is a holographic dual of the SYK model, in the sense of AdS/CFT, where you have a gravity theory on one side, and it is dual to a (conformally invariant) non-gravitational field theory on the other side. The key thing is that the gravitational theory has one dimension more than the field theory. I’ve spoken of such things a lot here on this blog so I won’t review, but instead let you dig a bit and find things to read in the archives. (You could put AdS/CFT in the search window, or maybe start here.)

Simply/glibly put, the duality says that some complicated (strongly coupled) dynamics of a field theory can be re-written as a simpler dynamics involving gravity, and the “re-writing” uses an additional spatial dimension. Most famously you have (super) Yang-Mills theory in 4D (which is conformally invariant, so let’s write it as CFT_4) being equivalent to a theory of gravity in 5D anti-de Sitter (AdS_5). So AdS_5/CFT_4. Many examples are known in various dimensions that fill out the pattern AdS_(d+1)/CFT_d. The picture I like to draw is of a ball (see above right), the interior of which is the AdS space where gravity is operating (I’ve cut a hole for you to see the inside), and the boundary of which has the (one dimension fewer) conformal field theory. You often hear people refer to the “boundary” and the “bulk” – well, that’s the picture.Important technical note: In the setup I drew above, the metric which measures spatial distances makes spacings smaller and smaller as you move out from the center, approaching zero as you get to the edge. This is another way of saying that the distance to the boundary is actually infinite. There are famous depictions of all this in 2D – MC Escher’s tessellations of the Poincaré disc (where now time is treated as a spatial coordinate too – we work with “Euclidiean signature”). See “circle limit III”, at the top of this post, to the right. The fish get smaller as you move out, but they’re really all the same size, allowing MC to draw an infinite space in a finite bit of paper.

So here, the SYK model is like the Yang Mills theory and the JT gravity is like the AdS. Well, that’s not quite right, and in fact the “not quite” is what makes it interesting, for many reasons. First of all, we should really stick to low energies, where it turns out the SYK model looks more and more like a quantum mechanics with a conformal symmetry, so it is “nearly” CFT_1. If it were all the way exactly conformally invariant, you’d want to say it was maybe dual to AdS_2. But it isn’t, and instead is dual to something that is “nearly” AdS_2. And it is the JT gravity that gets the “nearly” to work properly in the following well-defined sense. It is a model of gravity with a special coupling to a scalar field (a dilaton-like coupling, if you are familiar with the term) such that the equations of motion for the scalar enforce (as though it is a Lagrange multiplier) that the overall spacetime curvature is constant and negative (as AdS_2 has), but there is an important boundary term involving the scalar too. When that is properly handled it tells you that the boundary is allowed to fluctuate in shape, but its length is fixed to be \(\beta=1/T\).

There’s a nice picture of this. For two dimensions, that green ball representing AdS that we saw earlier is a disc (as we saw), and the sphere that’s the boundary of AdS is a circle. Looking at the picture (right), you can see that the ‘nearly’ AdS_2 aspect is the fact that the JT gravity’s boundary dynamics gives a boundary that is not out at the circle (where it would have infinite length), but that fluctuating shape of total length \(\beta\). (Notice that if the temperature goes to zero, then \(\beta\to\infty\) and so the whole thing heads toward being actually AdS_2, which makes sense.)Actually, your statement at the beginning of this post that there’s not much going on in gravity in 2D is correct, and so there’s not much in the way of gravity to talk about until you couple it to something. Here it is coupled to the scalar field, and the interesting dynamics is really all about that wiggling boundary. Turns out that it is governed by a “Schwarzian” form (see e.g. the lovely papers of Jensen, and Maldacena-Stanford-Yang) that follows from the way in which the \(T=0\) conformal invariance is broken, and it can be exactly solved, but I won’t go into that here as it will take me too far afield.

By the way, I’ve left out the names and papers of a lot more of the people who helped figure a lot of this out, but they are cited in my paper and the papers I cite there, so please have a look.

There are solutions of this 2D gravity model that can be interpreted as black holes in their own right, and there’s a lot of work on that, but it also describes black holes in higher dimensions (e.g., 4D charged or rotating), because the geometry near the horizon when the black hole is close to being extremal (so, at low \(T\)) is `nearly’ \(AdS_2\) (for the radial and time directions) times a simple manifold (e.g., a sphere, for the angular directions) of some overall volume that can fluctuate. The scalar sector of the JT gravity represents the dynamics of this volume. (There are some nice papers of Trivedi et. al. that explore this in detail – here’s one.) In this way the physics of SYK/JT can teach us about quantum aspects of black holes that are more realistic than such simple models are usually able to capture. The low temperature jiggling of the black hole degrees of freedom is reflected in the near-horizon geometry, and it is (in a well-defined approximation scheme) captured in the 2D model.

(Historical note, for the younger ones reading (which might be all of you since no serious grown-up reads blogs, right? 😉 ): Some of us (myself included) spent years some decades ago back in the 1990s studying string theory background geometries corresponding to black holes where this kind of decomposition happens. E.g. \(AdS_2\times S^2\) for charged black holes. But it was strictly at zero temperature. It was considered (rightly) a major bit of progress at the time to be able to find exact conformal field theory descriptions of 4D and 5D, etc., black holes in this near-horizon limit, compute string theory corrections to the geometries, etc. – this was long before AdS/CFT, where you might have first heard of near-horizon geometries, came along.)

(And by the way, JT gravity has been lurking in the literature since 1983/1984 – another great example of why its good to let people explore solid ideas even if they don’t immediately seem to have an application.)

In some ways, JT gravity is (part of) the answer for how to proceed beyond just the near-horizon geometry of a \(T=0\) black hole, and instead capture actual quantum dynamics where the degrees of freedom are allowed to do more than just sit there and be counted. (Counting is important too of course. The other major pre-AdS/CFT result from string theory and black holes was the Strominger-Vafa result showing how to count the degrees of freedom underlying the Bekenstien-Hawking Entropy, which at the time was best understood (again) at extremality, \(T=0\).)

Anyway, I think I’d better get back to other things for a bit. In part 2 of this, I’ll try to move the story forward a bit, including the part where I finally did pay attention to what was going on in this area, and discovered that things I’d been up to back in 1990 (!!), and that I’ve blogged about here a lot a decade or more ago, were highly relevant. In other words, I’d kind of been working on quantum black holes my whole career without realizing it!

-cvj

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