Take the 2-minute tour ×
MathOverflow is a question and answer site for professional mathematicians. It's 100% free, no registration required.

Hopefully, MathOverflow is the correct place for this. I had a student approach me and ask me what kinds of mathematics goes into the study of wormholes. She specifically asked whether there is any amount of topology involved, but I'd appreciate it if I could give her a more full answer. So, topology answers are the best but other areas of math would be nice. I am a topology Ph.D. student but know almost zero physics, just in case my background helps with your answer. Thanks.

share|improve this question
3  
physics.stackexchange.com seems like a more appropriate place for this. –  Qiaochu Yuan Apr 18 '11 at 19:56
    
@Qiaochu Yuan: I'll go try over there. I was just thinking that an answer from a math physicist might be better than from a physicist. –  Joe Johnson Apr 18 '11 at 20:00
    
google.com/… : Do you know that none of those results help (possibly because you already know what they say), or are you wondering if anyone here knows which of those results are good, or is it something else? –  Ricky Demer Apr 18 '11 at 20:25
2  
@Ricky Demer: When I did a search it seemed that all the results assumed I knew no math/physics or a whole lot of physics. I need an interpretation of the physics for someone who won't be scared of the math. –  Joe Johnson Apr 18 '11 at 23:04
1  
Another interesting paper that involves some topological issues is Misner's 1967 "Taub-NUT space as counterexample to almost everything". In particular, a solution to Einstein's equation is exhibited that, to make sense of its "maximal analytic extension", one may need to consider non-Hausdorff manifolds. –  Willie Wong Apr 19 '11 at 1:18

1 Answer 1

up vote 69 down vote accepted

A bit of General Relativity and Causality theory

One feature of general relativity is that the space-time is modelled as a Lorentzian manifold. The Lorentzian metric on the manifold has signature (-+...+), and thus distinguish between time-like, space-like, and null directions. A $C^1$ curve in your manifold is said to be time-like if its tangent vector is always time-like (similarly space-like/null).

For physical reasons we expect our manifold to be time-orientable: the set of time-like vectors in the tangent space has two connected components. We assume there is a continuous (non-vanishing) time-like vector field, which denotes the direction of "future".

A point $p$ is said to be in the chronological future of another point $q$ if there is a time-like, futurely directed curve originating from $q$ to $p$.

Asymptotic regions

For (possibly outdated by modern cosmological observation) physical reasons, one may assume that the local geometry of space-time far away from (large) gravitating bodies is nearly flat. Let $M$ be a Lorentzian manifold which for now we assume to be diffeomorphic to $\mathbb{R}\times \Sigma$, with the restriction of the metric on the $\Sigma$ leaves Riemannian. An asymptotic end of $\Sigma$ is a connected component of $\Sigma \setminus K$ for some compact set $K$ that is diffeomorphic to $\mathbb{R}^d\setminus B_1$. This induces a nice coordinate system on $M\setminus (\mathbb{R}\times K)$ (which allows us to talk about the radius function $r$). We make the flatness assumption (which can be justified by possibly enlarging $K$) that in each asymptotic region, future (or null) directed null rays $\gamma$ that remain in the asymptotic region for all parameter $s\in [s_0,\infty)$ will have $\lim_{s\to\infty} r(\gamma) = \infty$.

Fix now one asymptotic region, call it $M_\infty$. Its corresponding domain of outer communications $D_\infty$ consists of all points of $M$ which can be reached from $M_\infty$ by both a future time-like curve and a past time-like curve.

Intuitively speaking, each domain of outer communications is a connected region which can "communicate" with the asymptotic region through exchange of light-signals. In particular, it lies outside any black holes or white holes.

Worm holes

A simple description of a worm-hole space-time is just a connected Lorentzian manifold with multiple domains of outer communication.

For them to be of physical interest, we require there to exist a time-like or null curve originating from one domain of outer communication and ending in another. This represents the ability to send signals or even travelers between two "almost disjoint" regions of the universe.


So far it should be clear that you need some knowledge of differential/pseudo-Riemannian geometry at the very least to study worm holes.


The mathematical study of wormholes essentially boils down to writing down

  • Sufficient conditions to rule out their existence
  • Explicit examples of wormhole solutions

Let me start with the latter to motivate the former. The most classical solution to Einstein's equation in general relativity that admits a wormhole is the Reissner-Nordstrom charged black hole solution. This solution models a charged black hole, and the explicit analytic extension of the solution to the interior of the black hole reveal some possible structure. In particular, observers who fall into the black hole may not necessarily encounter a singularity in finite time (as opposed to the situation in Schwarzschild black holes). And based on the analytic extension, it is possible that such an observer will emerge after some time into another domain of outer communications by being spat out of a white whole.

Two key things to notice:

  • This worm hole is "one-way only"
  • I kept using the phrase analytic extension

As it turns out, under fairly generic conditions on the properties of the universe and the matters residing within it (in particular the dominant energy condition which also played a strong role in the Positive Mass Theorem of Schoen and Yau), worm holes can "only be one way". (Actually, with certain additional assumptions worm holes cannot even exist.) Results of this type are captured (as easy corollaries) under the name "Topological Censorship". The original version of the result states that the domain of outer communication must be (under certain reasonable physical assumptions) homeomorphic to $\mathbb{R} \times (\mathbb{R}^d\setminus B_1)$. A recent improvement by Galloway and collaborators states that (under reasonable physical assumptions including global hyperbolicity [more on which later]) any future directed time-like or null curve that starts from one asymptotic region and ends in another (a priori possibly different) asymptotic region must be entirely contained in one domain of outer communication. (Which basically states that wormholes don't exist unless you violate one of the physical assumptions; and if you remove global hyperbolicity, you can possibly obtain one-way worm holes.)

(There is also a much more classical result in the reverse direction: if a space-time admits a Cauchy hypersurface [a special type of a spatial slice] that has non-trivial topology, it must be geodesically incomplete [which suggests that there should be a black hole].)

The second issue at play is this analytic extension business. If you know a bit about the wave equation, please recall that it has the finite speed of propagation property. That is, when solving the initial value problem, the value of the solution at any given point in space-time depends can only on a compact sub-set of the initial space-like slice. (Or, in physical description, information does not travel faster than the speed of light.) Applying this to Einstein's equation of general relativity, one obtains the notion of "Maximal Globally Hyperbolic Extension" corresponding to a set of given initial data: the largest set in the space-time which is completely determined by the given initial data.

A priori, it is not clear whether the maximal globally hyperbolic extension can be further extended as a solution to the Einstein's equations. (Of course, such an extension will be non-unique, but it is interesting to ask whether they exist at all.) And in fact, in certain situations, more extension can be constructed by (real) analytic continuation of the solution. The case of Reissner-Nordstrom is one particular one, and it is due to this possible extension that we have the wormhole behaviour.

An open problem in mathematical general relativity is whether one can rule-out such extensions "generically". The "strong cosmic censorship conjecture" posits that the answer is positive: that the existence of such extensions requires the space-time to be conspiratorially nice.

Going back to the issue of constructing solutions/examples: as any example, to be physically meaningful, will be required to solve Einstein's equation, topological methods tend to be less useful in this context (unless you mean Gromov's h-principle), as geometry and analysis tend to be more "rigid" structures.


In classical mathematical GR, as you can see, topology has not come into play strongly. (The "problems" introduced by topology tend to be considered as pathological; lots of work were done in the 60s and 70s to discuss sufficient conditions to rule out such pathologies.) Differential/pseudo-Riemannian geometry and mathematical analysis (esp of PDEs) are generally used more heavily.

But that is not to say that topology has no role. It is more that the role of topology is much less clear, beyond the more simple applications of point-set topology, and some slightly less trivial applications based on connections between Riemannian geometry and topology.

In conclusion, let me give you some possible references if your student can be satisfied by black holes instead of wormholes. Some classical results to look into that in some way involves topology:

  • The Singularity Theorem of Hawking and Penrose (see, Wald, General Relativity; O'Neill, Semi-Riemannian Geometry will applications to relativity)
  • The Black Hole Topology Theorem (see this paper for the geometric aspects; the topological aspects requires knowing about the Yamabe problem)
share|improve this answer
9  
+1. Fantastic answer! –  José Figueroa-O'Farrill Apr 19 '11 at 2:37
3  
+1 Just Amazing... –  J Verma Apr 19 '11 at 3:52
2  
+1 Couldn't ask for a better answer. –  Joe Johnson Apr 19 '11 at 12:47
    
Another +1 for such a detailed and thoughtful answer! However, I'm confused by your statement that a spacetime is time-orientable if "the set of time-like vectors in the tangent space has two connected components." In signature $(-+\ldots+)$, won't each tangent space be isomorphic to $\mathbb{R}^{1,n}$, making this automatically true? –  Vectornaut May 15 at 2:22
1  
@Vectornaut: by tangent space I mean the total tangent space, not its pointwise fibre. So I mean $TM$ not $T_pM$. The point is that given that this is true pointwise, time-orientability is either true for the manifold itself or for a double cover. –  Willie Wong May 15 at 7:07

Your Answer

 
discard

By posting your answer, you agree to the privacy policy and terms of service.

Not the answer you're looking for? Browse other questions tagged or ask your own question.