Hyperbolic Methods for Einstein’s Equations
 2.3k Downloads
 50 Citations
Abstract
I review evolutionary aspects of general relativity, in particular those related to the hyperbolic character of the field equations and to the applications or consequences that this property entails. I look at several approaches to obtaining symmetric hyperbolic systems of equations out of Einstein’ equations by either removing some gauge freedoms from them, or by considering certain linear combinations of a subset of them.
1 Introduction
General Relativity (GR) is a peculiar physical theory. GR is about geometries, and not fields, in a given spacetime. That is, the theory’ solutions are not metric tensors or possible other matter tensors but rather the equivalence class of these tensors under arbitrary smooth relabeling of points in spacetime. This peculiarity makes the task of analyzing the dynamics of the theory difficult. One is used to evolving tensor fields, in fact tensor components, in a given coordinate system; while here the extra freedom of the theory makes these components nonunique. The values of some of these components can be given arbitrarily. Only certain relations between them are invariant and so have a physical meaning. In particular, some components can be made arbitrarily large and rough, while the geometry is, for instance, flat. Thus, it is often hard to see, from just comparing tensor components, whether two solutions, that is two geometries, are close to each other during evolution. To overcome this problem, several proposals have been made to fix the evolution in a unique way and at the same time obtain well behaved solutions. In general, these proposals provide for equation systems equivalent, in a sense to be discussed at length later, to Einstein’ equations which are hyperbolic, that is, whose evolution is continuous as a function of the initial data. This property is vital for many applications, ranging from Newtonian approximations to numerical simulations. The aim of this work is to review these proposals, paying special attention to the applications where they have proven fruitful.
1.1 Background and History
A simple example of a symmetric hyperbolic system is the wave equation, see Example I 2.2
Well posedness of the Cauchy problem for Einstein equations was established in the early fifties by ChoquetBruhat, [13], when the theory of evolutionary partial differential equations matured and general proofs for quasilinear hyperbolic systems became available. With further refinement of the general theory, it was possible in the early seventies to improve on the result by lowering the minimal differentiability required in the proof, thus allowing more general initial data sets, [42], see also [18] and [16, 27, 28]. These works used the harmonic gauge introduced by Lanczos in the twenties. For a discussion on the harmonic gauge see § 3.1

a) It established that the evolution equations preserved the asymptotic decay of the initial data. That is, if they initially were in some weighted space (for some specific weight factor) then, in any other time slice given in the development asserted by the theorem including boosted ones, the induced data on it was also in the same weighted space.

b) It established a relation between the size of the initial data in any bounded region and a lower bound for the time of existence of the solution, see [37] for a simple description.
Even more, it was possible to use as the function spaces for the initial data the same weighed spaces in which the constraint equations were solved, thus, for the first time obtaining a global (in space) control on Einstein’s equations.
All the power of the techniques used in the above mentioned body of work was not enough to get a result which most people suspected would hold: the existence of complete, asymptotically flat spacetimes for generic, although small, initial data. An idea which made a breakthrough on this problem was to regularize Einstein’ equations in terms of a conformally rescaled metric on the corresponding conformally compactified spacetime. Future and Null infinity are then at a finite distance, so standard, local in time, existence theorems can be used. Pursuing these ideas, Friedrich, [30, 29], was able to craft the full, and therefore nonlinear, Einstein equations for the conformal fields into a regular symmetric hyperbolic system, and so to create a formidable tool to study these problems. Earlier results using regularized equations for the conformal metric included the local linear stability of null infinity^{1}, [38].
The variables used range from frames to Weyl tensor frame components. The regularization of the full equations is complicated and requires appending to the original Einstein equations the Bianchi identities as a new and independent set of variables. For the first time, the harmonic gauge was not used. This was also the first time a symmetric system was obtained which was not the mere and standard translation of quasilinear second order wave equations into a first order system. This tool made it possible to show that, given any smooth and small enough initial data on a hypersurface reaching future null infinity at some cross section, a future development existed along which null infinity, to the future of such a hypersurface and up to future infinity, was included. A limitation of this technique is that initial data are not regular enough at spacelike infinity to make the estimates work there, and so a complete, asymptotically flat spacetime cannot be obtained, nor even a piece of null infinity starting from generic, although small, initial data on a spacelike hypersurface; nevertheless see [25].
A different path was followed by Christodoulou and Klainerman, [23]. They also made use of the detailed structure of Einstein equations, but in physical spacetime, to show global existence. The special structure of Einstein equations allows the use of other energy estimates beyond the traditional one. The estimates are boosted energies, [48, 49, 47], and are crucial to establishing this global result. Christodoulou and Klainerman did not use a conformal compactification of spacetime. They were able to obtain complete asymptotically flat spacetimes, i.e. asymptotically including spacelike regions, out of rather generic initial data in a Cauchy surface reaching that infinity. Christodoulou and Klainerman found that at null infinity the differential structure does not seems to be C∞. That is, they claimed there are smooth initial data sets whose development is not smooth at null infinity and that only finite differentiability remains. Christodoulou and Klainerman also did not use a harmonic gauge condition. Rather, their strategy was to use the equations for tensorial quantities built out of higher order derivatives of the metric. After obtaining estimates for these tensorial quantities, estimates for the metric and its first derivatives were obtained from elliptic theory, and the maximal slicing condition.
As expected, both methods used detailed properties of the Einstein equations to assert global existence of small data solutions. It is believed that both methods use the same properties, but with different techniques. That is, the property that allows the conformal Einstein equations to be regular should be the same property that allows boosted energies to be estimated. In fact both make estimates in terms of the BelRobinson tensor. However, to my knowledge, this has not yet been fully explored.
1.2 Main Subject and Plan of the Review
In the nineties, researchers have realized that other or more general forms of gauge conditions are needed to address some pressing problems, in particular, the numerical studies of regions of high curvature like black hole formation. One should also mention the study of slow solutions, that is, solutions which weakly depend on the value of the velocity of light in particular those which have a well behaved Newtonian limit. For the first problem, the issue has been whether the coordinate system chosen, that is, whether the gauge condition, stays well behaved during evolution and does not cause unphysical singularities, singularities which, for the numerical problem, are as bad as real ones. For the second problem, the issue has been whether the gauge is well behaved and does not prevent uniform continuity of slow solutions as the speed of light goes to infinity.
In both cases it is clear that one can choose bad gauges which would make the problem intractable and which nevertheless are genuine smooth coordinate conditions in the whole region of interest.

i) a solution to a hyperbolic equation, and so be incorporated as a part of the hyperbolic system;

ii) a solution to an elliptic equation, given a mixed hyperbolicelliptic system;

iii) a solution to a parabolic equation, given a mixed hyperbolicparabolic system;

iv) or it can be given as a fixed function in spacetime, chosen by a rule of thumb by looking at the initial data.
Each one of these possibilities can be implemented in a mathematically rigorous manner in most of the general schema proposed. And probably each of them would be of relevance in some specific implementation. The point, in other words, is that it is very difficult to go beyond a superficial or general description of the methods before some particular, extended, and fruitful use legitimizes the job.
In § 2 I give a short summary of hyperbolic theory, describing the case which is completely understood, namely the constant coefficient case, and mention what of it can be extended to the case of interest here, namely quasilinear systems. For physicists, this discussion should be a complement to Geroch’ lecture notes on symmetric hyperbolic systems [36]. This discussion follows very closely chapter II of [50], see also chapter IV of [39].
In § 3 I first describe the general problem of adapting the theory of hyperbolic systems to general relativity and the gauge issue. A companion to this section is, besides Geroch’ lectures, the paper of Friedrich in Hyperbolic Reductions [32]. In particular we discuss the standard approach, that is, the harmonic gauge.
In § 4 I present the more recent approaches, and divide them into four classes, according to the type of variables used.
In § 5 I compare the different implementations that have been made of the approaches introduced in the previous sections, and discuss the impact these approaches have had on the problems where they have been applied.
In § 6 I consider the role the constraint equations play in these new systems. In the harmonic gauge, constraint equations become evolution equations. The consistency of the gauge is all that is needed to ensure equivalence between Einstein’ equations and the harmonic system. In the new systems, one is not incorporating the constraints, and so one should make sure that, if the constraint equations are satisfied initially, they are satisfied during evolution. I claim that, in the initial value formulation, this follows from uniqueness of solutions to the equations and from the fact that the modified evolution vector fields proposed are tangent to the constraint submanifold. I also mention the difficulties that appear when considering an initialboundary value problem.
2 The Theory of Linear Constant Coefficients Evolution Equations and Generalizations to Quasilinear Systems
What follows is a short account of chapter II of [50], see also chapter IV of [39]. After this, I indicate what aspects of the theory generalize to quasilinear systems, and under which further assumptions this is so. I also give some indications of the relation of this theory to the stability issues of numerical simulations. This section can be skipped by those not interested in the mathematical theory itself or those who already know it.
2.1 Existence and Uniqueness of Smooth Solutions
Since the integral exists at each point, it can be differentiated inside the integral sign where it gives another compactly supported integrand, thus these functions are smooth (C∞(ℜ^{n}). What’s more, since the PaleyWiener theorem holds, they are analytic.
 i)
u(⋅;,t) ∈ M_{0} for all t ≥ 0;
 ii)
its Fourier transform, û(ω,t), is continuous, and vanishes for ‖ω‖ > k where k is some constant independent of t;
 iii)
u is a classical solution; that is u_{t} exists and u satisfies the equation at each point (x,t).

It is possible to define weaker conditions for well posedness in which the norm for the initial data is different (weaker) than the norm for the solution. This is unsatisfactory for equations in which there is no preferred time direction. Besides, in general it produces results which are not robust under lower order term (in differentiation) perturbations of the equations, and so do not generalize to variable coefficients or nonlinear equations.

Defining continuity through norms is a limitation and rules out certain more general types of hyperbolicity conditions, in particular those due to Leray and Ohya, [54, 55], see more below.

Well posedness and linearity imply that we can extend by continuity the set of solutions to all those which are generated by initial data on the completion generated by M_{0} on the given norm.
 i)
The system is L^{2} well posed.
 ii)
There exist constants k, and a, and a positive definite Hermitian form H(ω) such that:
2.2 First Order Systems
If A^{a} satisfies the above condition for some H(ω), then we say that P(D) is strongly hyperbolic, which, as we see, is equivalent for first order equation systems to well posedness. If the operator H does not depend on ω_{a}, a case that appears in most physical problems, then we say the system is symmetric hyperbolic. Indeed, if H does not depend on ω_{a}, then there is a base in which it just becomes the identity matrix. (One can diagonalize it and rescale the base.) Then the above condition in the new base just means that A^{a}ω_{a} with the upper matrix index lowered is symmetric for any ω_{a}, and so each component of A^{a} is symmetric. Even in the general (strongly hyperbolic) case, one can find a base (ω_{a} dependent) in which P(iω) can be diagonalized, basically because it is symmetric with respect to the (ω_{a} dependent) scalar product induced by H(ω). In this diagonal version, it is easy to see that the well posedness requires all eigenvalues of iA^{a}ω_{a} to be purely imaginary. Thus we see that an equivalent characterization for well posedness of first order systems is that their principal part (i.e. order systems is that their principal part (i.e. iA^{a}ω_{a}) has purely imaginary eigenvalues, and that it can be diagonalized by an invertible, ω_{a}dependent, transformation. The classical example of a symmetric hyperbolic system is the wave equation.

A first order system is called weakly hyperbolic if the eigenvalues of the principal part are purely imaginary. This condition, clearly weaker than strong hyperbolicity, is not enough to assert well posedness in the sense I have defined here, and so I do not discuss it further.

A first order system is called strictly hyperbolic if all eigenvalues of the principal part are purely imaginary and distinct. If the eigenvalues are distinct, then the eigenspaces invariant under the action of P_{1}(iω) are one dimensional and the system can be diagonalized. Thus this class is contained in the strongly hyperbolic one. Due to the degeneracies of systems induced by symmetries in more than one dimension, physical problems are seldom strictly hyperbolic. Sometimes this definition is used to mean that the eigenvectors belonging to the different invariant spaces generated by the symmetries, which must be also invariant under iA^{a}w_{a}, have distinct eigenvalues. With suitable conditions on the symmetries, this implies the full diagonalization of the principal part, and so equivalence with strong hyperbolicity.

There is a slightly different notion of hyperbolicity due to Leray see [54] and [55]. There a system is called strictly hyperbolic, or just hyperbolic, if it satisfies certain conditions which amount to having the Cauchy problem well posed in the sense we have used. A system is called nonstrictly hyperbolic if it satisfies conditions implying well posedness of the Cauchy Problem, but where the continuity notion is not given by a norm, but rather through Gevrey classes of functions. In particular these spaces are subspaces of smooth, C^{∞} functions, and so the data must be also smooth. I doubt very much can be done with them in terms of studying the stability of numerical methods, so we shall not concentrate on them.
2.3 Generalization to Variable Coefficient and Nonlinear Systems
Systems of this type are called quasilinear because the derivative appears linearly. This property allows one to use most of the machinery for constant coefficient equations to prove well posedness, thus the local existence is well understood, via linearization techniques. There are few global results, and in general they depend on more refined knowledge of the equation systems for which they apply.
The behavior of solutions to quasilinear equations is not yet fully understood. Most of the solutions develop singularities in a finite time for most initial data, even if they are in M_{0}. This is the case for convective systems, or more generally for genuinely nonlinear systems, see [46, 57], for the definition and main results, a class which includes systems like perfect fluids and relativistic dissipative fluids for they contain as part of the system the perfect fluid equations. This is also the case for general relativity, where singularity theorems (see [41, 60]) tell us about the development of singularities, although of a different type. Thus the concept of well posedness has to be modified to account for the fact that solutions only last for a finite time and this time depends on the initial data. Basically, the most we can pretend to show in the above generality is the same type of well posedness one requires from an ordinary system of equations. Which is quite a lot! The nonlinear aspect of the equations implies also that it is not possible to generalize their solutions to be distributions. The minimum differentiability needed to make sense of an equation depends on the particular equation. Furthermore, there are cases (e.g. convection) in which, for some function spaces of low differentiability, the equation makes sense and some solutions exist, but they are not unique^{3}.
Definition 4 Let u_{0}(t,x), t ∈ [0,T_{0}), T_{0} < +∞ be a smooth solution of a quasilinear evolution system. We shall say the system is well posed at the solution u_{0} with respect to a norm ∥ ∥ if given any δ > 0 there exists ɛ > 0 such that for any smooth initial data f(x) such that ∥ff_{0}∥ > ɛ, with f_{0}(x):=u0(0,x) There exists a smooth solution u(t,x) defined in a strip 0≤t≤T, with u(t,⋅;)u_{0}(t,⋅)<δ,TT_{0}<δ.
In order not to worry about the possibility that the smoothness of the solutions be too stringent a requirement, one can smooth out the equation using a one parameter family of mollifiers, and require that the relation δ(ε) be independent of that parameter family.
To obtain results about well posedness, we just have to slightly modify the concepts of hyperbolicity already discussed in the constant coefficient case. Since in the constant coefficient case the matrices did not depend on the points of spacetime, nor on the solution itself, we had only two cases. In one case, the norm H did not depend on ω_{a}, and so in some base the matrix A_{a} was symmetric. In the other case, the norm H did depend on ω_{a}, and we had a general strongly hyperbolic system. In the latter case, it can be seen that H(ω) is piecewise continuous and so integrable, which is, in that case, all that is needed to proceed with the proof. In the general case with which we are now dealing, H would in general depend not only on ω_{a}, but also on the point of spacetime and on the solution, H = H(ω_{a},t,x,u).
This difference has caused terminology to be not uniform in the literature, so I have taken advantage of this and establish terms in the way I consider best suited for the topic.
Certain authors call some systems symmetric hyperbolic and others symmetrizable. They call symmetric hyperbolic only those systems where the symmetrizer does not depend on the unknown variables nor on the spacetime variables (or at most depends only on the base space variables H := H)(t,x); they call the other systems symmetrizable. This is a rather arbitrary distinction, since the methods of proof used are valid for both with no essential difference. Thus, if H does not depend on ω_{a} but depends smoothly on all other variables, H := H(t,x,u), then we shall still say the system is symmetric hyperbolic. In this case the nonsingular transformation which symmetrizes A^{a}(t,x,u) is smooth in all its variables.
The existence and smoothness proof is based, as in the constant coefficient case, on energy norm estimates, but now supplemented by Sobolev inequalities. Since the norm is built out of H and it does not depend on ω_{a}, no passage to Fourier space is needed.
If H does also depend on ω_{a}, and is smooth on all variables, H := H(t,x,u,ω_{a}), we shall say the system is strongly hyperbolic. The existence and smoothness proof now requires the construction of a pseudodifferential norm out of H, and so pseudodifferential calculus is needed, which implies that H has to be smooth in all its entries, in particular in ω_{a}.
We shall not discuss weak hyperbolic systems, for they are generically unstable under perturbations, nor shall we discuss strictly hyperbolic systems, i.e. systems with strictly different eigenvalues of A^{a}ω_{a}, for they seldom appear in physical processes in more than one dimension.

In the generic case the value of r cannot be reduced from the above value, but of course it can for certain special types of systems. In general relativity, a slight improvement, \(\left( {r\; > \frac{n}{2}} \right)\), is obtained from the fact that the matrix Aa only depends on a subset of variables (the metric).

The time of existence is the same for all r. That is, when a solution loses differentiability, it loses all of it at the same time. This is reflected in the following result: [58]. If a solution exists until T_{0} and there ∥u(t,⋅;)∥_{C} _{★} ^{1} is bounded, (where C _{★} ^{1} is a Zygmund space, see Appendix A in [58]), then the solution can be extended further. Again in general relativity a slight improvement can be obtained, see [42], and [18].
2.4 Hyperbolicity and Numerical Simulations
Knowing that the field equations for GR can be cast in a symmetric hyperbolic form, we can now ask how this fact can be of help for numerical calculations, (besides the extremely important fact that the problem would be well posed and so tractable!). There are at least two reasons why one should use variables in which the system is hyperbolic when performing numerical simulations. The first reason is that having a strongly hyperbolic system allows for standard constructions of numerical codes which are stable. If the system is symmetric, hyperbolic codes with better properties can be constructed. In particular, schema for symmetric hyperbolic systems can be constructed with numerical dissipation of lower order than what is needed for generic strongly hyperbolic ones (see chapter VI of [39]). In variables where the system becomes diagonal, one can also use methods which take advantage of that structure.
The second reason for using a hyperbolic formulation for numerical analysis is that well posedness of the system gives bounds on the growth of the solution and its derivatives, as long as the solution is smooth^{4}. This property, when used in conjuction with stable algorithms, implies that one can bound the errors made on the simulation. That is, one knows not only that the error goes to zero as some power of the step size, but also the proportionality factor of that power law. In simulating phenomena whose observation would require hundreds of millions of dollars, a tight control of the accuracy reached should be required. Nevertheless it should be noted that raw hyperbolicity estimates alone usually give exponential bounds with very large growth coefficients, and that they are not of much value for numerical work.
Many of the systems we shall analyze can be cast as flux conservative equations with sources. This is a direct consequence of the facts that the principal part of the equations depends only on the metric variable, and that the equation for the time derivative of it does not contain derivatives of any of the dynamical variables. This property is important when using codes with variable grid spacing, even more if one considers that there are many standard codes for fluids which are truly flux conserving with adaptive grid schema.
It has to be said that flux conservation is important when dealing with systems that develop shock waves, that is in convective or more precisely in genuinely nonlinear systems (for a definition of this term and many of the results, see [46, 57]). One should be cautious about any expectation of improvement by using flux conservative properties in general relativity, since here the shocks would probably not develop in particular the systems are not genuinely nonlinear. Rather, when singularities appear, they would be much worse than mere discontinuities of some of the dynamical fields.^{5} Due to bad gauge choices, discontinuities resembling shocks have been observed in numerical simulations, see [5]. Perhaps, instead of trying to devise an algorithm which allows one to go through these discontinuities, one should concentrate on finding better gauges, where it could even happen that the system cannot be put in flux conserving form. Thus, it is not clear whether flux conservative forms are relevant for vacuum general relativity.^{6}
Going Further For the reader wishing to delve further into this precious theory of hyperbolic systems, while keeping a physicist’s approach, I recommend [36]. For those wishing to see more of the machinery at work, I recommend the book of Kreiss and Lorentz [50]. Finally, for those who really want to get the latest on the technical aspects and the modern approach to the problem, I recommend Taylor’s book, [58]. Considerations about numerical analysis and algorithms can be found in [39]. In particular, that book contains general stable algorithms for strongly and symmetric hyperbolic systems and numerical error bounds in terms of analytic bounds of the exact solutions applicable to nonlinear systems.
3 The Problem of Hyperbolicity in General Relativity
What follows are descriptions of the problem of hyperbolicity in general relativity and of the main approaches that have been proposed to deal with the problem.
In studying Einstein’s field equations we are faced with a problem (see [23, 36, 32]): While the theory of partial differential equations has developed as a theory for tensor components in a given coordinate system, or at best for tensor fields in a given metric space, Einstein’s equations acquire their full meaning and the characteristics which distinguish them from all other physical theorieswhen they are viewed as equations for geometries, that is, for equivalent classes of metric tensors. The object of the theory is not a metric tensor, but the whole equivalence class to which it belongs all other metrics related to the first one by a smooth diffeomorphism. This fact is contained in the equations, for they are invariant under those diffeomorphisms. To clarify the concept, and see the problem, let us assume we have a solution to Einstein equations in a given region of a manifold. Take a spacelike hypersurface across it, Σ_{0}, and a small “lens shaped” region which can be foliated by smooth spacelike surfaces Σ_{t} starting at Σ_{0}. If Einstein’s equations were hyperbolic for the metric tensor, then uniqueness of the solution (the metric tensor) in the lens shaped region would follow from the standard theory once proper initial data at Σ_{0} is given. But we know that if we apply a diffeomorphism to the original metric tensor solution, which is different from the identity only in a region inside the lens shaped one but which does not intersect the initial Σ_{0} slice, the resulting metric would also satisfy Einstein’s equations, thus contradicting uniqueness, and so the possibility that the system be hyperbolic.
Since, as shown in § 2, hyperbolicity is equivalent to the existence of norms which are bounded under evolution, we see that for Einstein’s equations there cannot be such norms on the space of metric tensors. Norms are not only important for well posedness, but also for other related issues which often appear in general relativity, in particular when one tries to see whether some approximation schema is indeed an approximation. Examples of this appear in very unrelated cases, for instance, in numerical algorithms and postNewtonian approximations. Thus, a method is needed to find relevant norms on metric tensors, that is, to break the diffeomorphism invariance. The norms thus obtained are not natural, and so by themselves do not imply any physical closeness of metrics in numerical values. They have to be considered in their topologically equivalent class. Physically relevant notions of closeness can still be obtained by building, out of the metric tensor and its derivatives, diffeomorphism invariant quantities and making the comparisons with then.
Can we avoid this detour into tensors and make a theory of diffeomorphism invariant objects? It is not clear whether this can be done. Some attempts in this direction have been made by trying to build norms which have some partial diffeomorphism invariance. Here the norms are made out of scalars built out of curvature tensor components of the metric, in particular see [23, 32]. But I think a fully geometrical theory needs other types of mathematics than the theory of partial differential equations, a theory which might be emerging from parallel questions in quantum gravity.
3.1 The Standard Approach, or the 4D Covariant Approach
The standard approach to overcome this problem has been to “fix the gauge”, that is, by imposing some extra condition on the metric coordinate components which would select one and only one representative from each equivalent class of Einstein’s geometries. With a clever choice of gauge fixing, commonly the socalled harmonic gauge, Einstein’s equations can be “reduced” to a hyperbolic system by removing from them the parts which the gauge condition would make vanish. This reduced system is equivalent to the full Einstein equations if one can prove that, possibly after imposing further initial data set constraints, the solutions of the reduced system satisfy the gauge conditions previously imposed to the system. Alternatively, one can think of this method as fixing some components of the tensor obtained by taking the difference between two connections, the one associated with the metric tensor at which we are looking and the one associated with some other arbitrary background metric [26, 41].
A convenient way to describe this scheme is by introducing a background metric, ̃g^{ab}, thus the gauge is not a coordinate condition, but rather a condition which links the physical metric with the background one. In this approach, see [41], the basic variable is a densitized symmetric tensor, Φ^{ab} := gδg^{ab}, where g is the metric determinant with respect to the background one, ^{7} and δg^{ab} := g^{ab}  ̃g^{ab}.
In that gauge, Einstein’s equations are “reduced” to a hyperbolic system by removing from them all terms containing Ψ^{a}, for this quantity is assumed to vanish in this gauge. By doing this one gets a set of coupled wave equations, one for each metric component. Thus by prescribing at an initial (spacelike) hypersurface values for Φ^{ab} and of its normal derivatives one gets unique solutions to the reduced system. When are such solutions solutions to Einstein’s equations?
That is, under what conditions does Ψ_{a} vanish everywhere? It turns out that the Bianchi identity grants that when Φ^{ab} satisfies the reduced equations, then Ψ_{a} satisfies a linear homogeneous second order hyperbolic equation. Standard uniqueness results for such systems implies that if initially Φ^{ab} is chosen so that Ψ_{a} and its normal derivative vanish at the initial surface, then they vanish everywhere on the domain of dependence of that surface. Thus the question is now posed on the initial data, that is, on whether it is possible to choose appropriate initial data for the reduced system, (Φ^{ab}, ̇Φ^{ab}), in such a way that (Ψ_{a}, ̇Ψ_{a}) vanish initially. It turns out, using that the reduced equations are satisfied at the initial surface, that one can indeed express Ψ_{a} and its normal derivative at the initial surface, in terms of Φ^{ab} and its derivatives (both normal and tangential to the initial surface). Thus one finds there are plenty of initial data sets for which solutions to the reduced system coincide with solutions to the full Einstein system. Are they all possible solutions to Einstein’s equations, or are we loosing some of them by imposing this scheme? The answer to the first part of the question is affirmative (subject so some asymptotic and smoothness conditions), for one can prove that given “any” solution to the Einstein equations, there exists a diffeomorphism which makes it satisfy the above harmonic gauge condition.
It is important to realize that it is not necessary to set Ψ_{a} a to zero to render the Einstein equations hyperbolic; it just suffices to set it equal to some given vector field on the manifold, or any given vector function of the spacetime points and on the metric, but not its derivatives. So there are actually many ways to hyperbolize Einsteins’s equations via the above scheme. We shall call all of them harmonic gauge conditions, and reserve the name full harmonic condition to the one where Ψ_{a} = 0.
An important advantage of this method is that some gauge conditions, like the full harmonic gauge, are fourdimensional covariant although a background metric is fixed a condition which can be very useful for some considerations.
One drawback of this method, at least in the simplest version of the harmonic gauge, i.e. the full harmonic gauge, was recognized early, [14]. The drawback is the fact that this gauge condition can be imposed only locally, and generically breaks down in a finite evolution time. A related problem has been discussed recently in [5] in the context of the hyperbolizations of the ADM variables with the harmonic gauge along the temporal direction. The above disadvantage can be considered just a manifestation of another: the lack of ductility of the method, that is the fact that one has been able do very little besides imposing the full harmonic gauge condition, and that for each new harmonic gauge condition one would like to use, a whole study of the properties of the reduced equations would have to be undertaken. Although there are many other gauge conditions besides the harmonic one, the issue of the possibility of their global validity, or the search for other properties of potential use, do not seem to have been considered. For a detailed discussion of this topic, see [31, 32], and also [41].
One can summarize the situation by noticing that in this setting one needs to prescribe a four vector as a harmonic gauge condition. Since the theory keeps its four dimensional covariance, then it is hard to choose any other vector but zero, that is the full harmonic gauge. Since recently there have been no advances in this area, I do not elaborate on it.
3.2 The Modification of the Field Equations Outside the Constraint Submanifold, or the 3+1 Decomposition Point of View
Another approach to deal with the diffeomorphism freedom of Einstein’s equations is by first removing the diffeomorphism invariance. This is done by prescribing the time foliation along evolution, that is, by prescribing a lapseshift pair along evolution. This removes the diffeomorphism invariance up to threedimensional diffeomorphisms at the initial surface. Sometimes four dimensional covariance is also broken by splitting Einstein’s equations, and possibly other supplementary equations, with respect to that foliation, and then recombining the split pieces in a suitable way. The resulting equations are equivalent to the original ones for it is just a linear combination of them so they have the same solutions. Notice that here we are doing more than just a 3 +1 decomposition, since in general one is recombining spacespace components of the Einstein tensor with timetime, and timespace components in a noncovariant way, and taking as equations this combination, or even transforming the equations to first order in derivatives of the variables by defining new variables and equations and modifying them.
After this procedure is done, one obtains a system which is symmetric hyperbolic for most choices of given lapseshift functions, once they are suitably rescaled. Subsequent arguments go very much on adding equations for the lapseshift vector in order to make the whole system well posed, and presumably useful for some application. It is instructive to think of these modifications of the evolution equations from the point of view of the initial value formulation. There one starts by solving the constraint equations, the timetime and timespace components of the Einstein tensor, at the initial surface. With the initial data thus obtained, one finds the solution to the evolution equations which are taken to be the spacespace components of the Einstein tensor. Since that evolution preserves the constraints, (The vector field generating the flow in phasespace is tangent to the constraint submanifold.), one can forget about the constraint equations and think of the evolution equations as providing an evolution for the whole phasespace. In this sense, the modification one is making affects the evolution vector outside the constraint submanifold, leaving the vector intact at it. Uniqueness of solutions, which follows from the well posedness of the system, then implies that the solutions stay on the submanifold. Nevertheless, and we shall return to this point, as shown in [33], there is no guarantee that the submanifold of constraint solutions is stable with respect to the evolution vector field as extended on the whole phasespace. This is an important point for numerical simulations.
4 Recent Approaches to the Problem
4.1 The ADM representation
In the ADM formulation of Einstein’s equations, the fields involved are detached from the underlaying spacetime and brought into an abstract three dimensional manifold product a segment of the real line. To obtain the relation between these abstract fields and the metric tensor defining a solution of Einstein’s equations, we start by pretending we have such a solution, that is a spacetime (M,g_{ab}). In this spacetime we look at a Cauchy surface, Σ_{0}, that is, an everywhere spacelike hypersurface such that any inextendible timelike piecewise smooth curve pierces it once and only once, and a time flow, that is, a smooth timelike vector field, t^{a}. From the definition of the Cauchy surface, t^{a} is never tangent to it and every point of M falls in an integral curve of t^{a}. Thus, in assuming the existence of Σ_{0} we are restricting attention to manifolds of the type S × ℜ. To make this structure more apparent we define a function t by setting to zero the parameter defining the integral curves of t^{a} at Σ_{0}, that is, the value of t at p ∈ M is defined as the value of the parameter the integral curve of t^{a} takes at p if defined in such a way that at Σ_{0} is takes the value 0. We shall call the surfaces of constant t by Σ_{t}. Thus t^{a}∇_{a}t = 1, notice that nevertheless, in general, they are not spacelike. When they are spacelike, we shall call t a time function. In this case we also say we have a spacelike foliation of spacetime (M, g^{ab}). We shall assume that this is the case, but one must take into account that when we are solving for a spacetime we do not know for how long this would continue to hold. Using this structure we can split tensor into “space” and “time” parts with respect to the surfaces Σ_{t}. If n^{a} is the normal to them, that is, \({n^a}\;: = \;  {g^{ab}}\frac{{{\nabla _b}t}}{{\sqrt {{g^{cd}}{\nabla _c}t{\nabla _d}t} }}\) then h^{ab} := g^{ab}n^{a}n^{b} is the induced metric on each Σ_{t}. We also define the lapse shift pair, (N, N^{a}), as the “timelike” and “spacelike“ parts of t^{a} with respect to Σ_{t}, that is, t^{a} := Nn^{a} + N^{a}.
Given the foliation, and the triad (h^{ab}, N, N^{a}) we can reconstruct the metric as g^{ab} = h^{ab}  N^{2}(t^{a}  N^{a})(t^{b}  N^{b}). Given another foliation, (Σ_{0},t'^{a}), but the same triad, we get another metric tensor, the relation between both is a diffeomorphism which leaves invariant Σ_{0} and is generated by the integral curves of t^{a}  t^{'a}. Alternatively we can choose another pair (N, N^{a}) and so construct another metric tensor, the relation between both metric thus obtained is also a diffeomorphism. Since one is interested in geometries, that is in metric tensors up to diffeomorphisms, both metric obtained are equivalent, but one needs to pick up an specific one in order to write down, (and solve), Einstein’s equations.
Note that there are two “dynamical” variables, h_{ab}, and P^{ab}, while the lapseshift pair (N, N^{a}), although necessary to determine the evolution, is undetermined by the equations. Note also that they do not enter into the constraint equations, for as said above a change on the lapseshift pair leave the fields at initial surface unchanged.
It is important step back now and see that these equations can be thought as “living” in a structure completely detached from spacetime. To see this, identify all points laying in the same integral curve of t^{a}, thus the equivalence class is a three dimensional manifold S, homeomorphic to any Σ_{t}. On it, for each t we can induce spacecontravariant tensors, such as h_{ab}(t), P_{ab}(t), N_{a}(t), and scalars, as N(t). As long as the surfaces are spacelike, the induced metric is negative definite and we can invert it, thus we can perform all kinds of contractions and write the above equations as dynamical equations on the parameter t on fields on the same manifold, S. This is of course the setting in which one sets most of the schemes to solve the equations, and it is hard to keep control, even awareness, that the surfaces defining the foliation can become null or nearly so. Einstein’s equations “feel” that effect since they are causal, and this is abruptly fed back via the development of singularities on the solutions . They do not have any thing to do with real singularities of spacetime, but rather with foliations becoming null.
The first application of this idea to Einstein’s equations appears to have been [19]. There a hyperbolic system consisting of wave equations for the time derivative of the variable hh^{ab} is obtained when the shift is taken to vanish and the lapse is chosen so as to impose the time component of the harmonic gauge. The shift is set to zero, but, as stated in the paper, this is an unnecessary condition. Thus, it is clear that one gains in flexibility compared with the standard method above. This seems to correspond with the fact that in one of the equations forming the system, the time derivative of the evolution equation for the momentum, the momentum constraint has been suitably added, thus modifying the evolution flow outside the constraint submanifold. As stated in the paper, they could not use the other constraint, the Hamiltonian one, to modify that equation.
Although in the introduction of [19] there is a remark dedicated to numerical relativists about the possible importance of having a stable system, the paper did not spark interest until recently, when applications required these results to proceed. In recent years, a number of papers have appeared which further elaborate on this system, [2, 4, 1]. In particular I would like to mention [4], where the authors look at the system in detail, writing it as a first order system, and introduce all variables which are needed for that. In these recent papers, the generalized harmonic time gauge has been included, as well as arbitrarily prescribed shift vectors. If one attempts attempts to write down the system as a first order one, that is, to give new names to the derivatives of the basic fields until bringing the system to the form of equation 1, the resulting system is rather big, it has fifty four variables, without counting the lapseshift pair. We shall see that there are first order hyperbolic systems with half that number of variables.
Two similar results are of interest: In [9] a system is introduced with basically the same properties, but of lower order, that is, only first derivatives of the basic variables are taken as new independent variables in making the system first order. In this paper, it is realized that the same trick of modifying the evolution equations using the constraints can be done by modifying, instead of the second time derivative of the momentum, the extra equation which appears when making the ADM equations a first order system, that is the equation which fixes the time evolution of the space derivatives of the metric, or alternatively the time evolution of the Christoffel symbols. When this equation is suitably modified by adding a term proportional to the momentum constraint, and when the harmonic gauge in the generalized sense used above is imposed, a symmetric hyperbolic system results. In [11] the generalized harmonic time gauge is included, as well as arbitrarily prescribed shift vectors. For the latest on this approach see, [10]. I shall comment more on this in next section, § 4.
In [32] a similar system, in the sense of using variables from the 3+1 decomposition, is obtained by imposing also the same generalized harmonic time gauge. This system, as is the original system of [19], is of higher order because it includes the electric and magnetic parts of the Weyl tensor in the 3 + 1 decomposition. As such, it contains more variables (fifty) than the two discussed above (thirty).
4.2 The Frame Representation
Another way of dealing with Einstein equations is through the frame representation. There, instead of using the metric tensor as the basic building block of the theory, a set of frame fields is used. At first this representation seems to be even less economical than the metric tensor representation of geometries, since, on top of the diffeomorphism freedom, one has the freedom to choose the frame vector fields. In short, one has sixteen variables instead of ten. But the antisymmetry of the connection coefficients compared with the symmetry of the Christoffel symbols levels considerably the difference, ending, after adding the second fundamental form and others, with twentyeight variables, instead of the thirty of the conventional system. But this count is not entirely correct. As mentioned above, in order to close the system of equations one has to add the evolution equations for the electric and magnetic part of the Weyl tensor, thus ending with a total of thirty four variables. Actually one can close the system with the twenty four variables at the expense of making the equations into second order wave equations, (See for instance [59].), so effectively adding more variables when reexpressing it as a first order system.
The more important application of the frame representation has been the conformal system obtained by Friedrich, [30, 29], (see § 1), where in a fixed gauge he got a symmetric hyperbolic system which allowed him to study global solutions. Later, using similar techniques and spinors, he found a symmetric hyperbolic system with the remarkable property that lapse and shift appear in an undifferentiated form, allowing for greater freedom in relating them to the geometry without hampering hyperbolicity [31]. In [32] he introduces new symmetric systems for frame components where one can arbitrarily prescribe the gauge functions, which in this case does not only include the equivalent to the lapseshift pair, but also a three by three matrix fixing the rotation of the frame. In this case, these gauge functions enter up to first derivatives. This compares very favorably with the ADM representation schema where the lapseshift entered up to second order derivatives. Friedrich also finds a symmetric hyperbolic system with the generalized harmonic time condition. Contrary to the systems in the ADM formalism, where the issue is rather trivial, these systems do not seem to allow for a writing in flux conservative form. We do not consider that a serious drawback. The structure of Einstein’s equations is very different than those of fluids, where the unavoidable presence of shocks makes it important to write them that way. Indeed the reason fluids have shocks can be attributed to their genuinely nonlinear character, [46], a property not shared by Einstein‘s theory. (More about this in the next section, § 4.)
4.3 Ashtekar‘s Representation
The two possible values α can take correspond to the two characteristic directions the wave equation defines. This trick can not be extended two more dimensions, basically because the space derivative of ϕ is a vector, and so can not be properly mixed with its time derivative. But in other dimensions one can implement similar schema if the fields are not scalars but appropriate tensors.
Einstein’s equations in Ashtekar’s’ variables [7, 8] is one beautiful example of this, since they have the remarkable property of naturally constituting a first order evolution system. Because of this reason it is also a compact system with twentyseven unknowns, even before imposing the reality condition on the connection variable. Recently it has been proven [45] that such a system is symmetric hyperbolic if suitable combinations of the constraint equations are added to their evolution equations, thus effectively changing the flow outside the constraint submanifold of phasespace.
In Ashtekar’s representation the basic variables are a densitized SU(2) soldering form, ̃σ^{a}A^{B} and a SU(2) connection A_{aA}^{B} which are tangent to a spacelike foliation of space time determined by given ‘lapse’shift pair Ñ = N/detσ, N^{a}.
Note that the principal part of the system is block diagonal and the eigenvectorseigenvalues are very simple combinations of ̃σ with the elements of an orthogonal basis {ω^{a},m^{a},̄m^{a}}, where ω^{a} is the wave vector.
In this new system, the ‘lapse’shift pair can be chosen arbitrarily. But in fact the ‘lapse’ that appears here is a scalar density which has already incorporated the square root of h on it. So the freedom is actually the same as in the ADM representation. As in the frame representation, the lapseshift pair appears only with derivatives up to first order. In this case it is relatively easy to see the freedom in making up evolution equations for the lapseshift pair. As said above, the system is symmetric for Ashtekar’s variables, since the lapseshift pair enters as terms with up to first derivatives, one can take those terms from the nonprincipal part of the system and promote them into the principal part of a bigger system which incorporates the lapseshift as extra variables. Thus, these terms constitute an offdiagonal block of the bigger principal part matrix. Imposing symmetry to the bigger matrix fixes the opposite offdiagonal part of the matrix. The only freedom left is on the lapseshift blockdiagonal part, which can be chosen to be any symmetric matrix we like. The nonprincipal part of the equation system on the lapseshift sector can also be chosen arbitrarily. Of course, in contrast with the ADM representation results, one can also choose a gauge condition via elliptic equations on the lapseshift pair. In this case, the elliptic system can be of first order in the lapseshift or related variables. For instance, one could use Witten’s equation to evolve them.
As we have seen, the generalized harmonic time gauge seems to appear naturally in most attempts to get well posed evolution systems. Thus it seems to be really a key ingredient, perhaps with some physical content. One could argue in that direction from the circumstances in which it appears in [34], namely effectively improving the estimates of the behavior of solutions admitting a Newtonian limit that is in a way related to the longitudinal modes of the theory. This longitudinal modes are part of the evolution, although they are not expected to behave in a hyperbolic manner. See also the comments around equation (9) in [10].
5 Beyond the Prescribed Gauge
In this section we will look at several attempts to, once a hyperbolic system has been obtained for the evolution variables, extend it into a bigger well posed system where the lapseshift pair, or more generally the gauge variables of a particular system, can be determined by some prescription which in general depends on the dynamical variables. The bigger system does not need to be hyperbolic, it only needs to be well posed, and so for instance it can be mixed elliptichyperbolic.
5.1 Trial and Error Method
One alternative would be to start with some arbitrary prescription for the gauge variables, evolve the solution for a while, stop, look for troublesome regions, and modify the gauge prescription there. One would do that only a finite number of times and choose smooth prescriptions and smooth transitions between them, so no problem of well posedness or numerical stability would be created by that procedure. With some experience, and luck, this procedure could work.
Perhaps the mayor drawback of this approach is the fact that the strict harmonic gauge, the most conspicuous choice, does not behave well under evolution. This has been known for a long time [14], and more recently new indications have been found in [5]. These findings are of course not valid for the generalized harmonic time gauge because one can trivially take any solution, draw a well behaved foliation on it, and identify the generalized gauge that works for that solution. Some attempts have been made in order to get loose from the generalized harmonic time condition, presumably with the intention of later imposing equations on the free variables, otherwise independent fields. In [3] a nonstrictly hyperbolic system is found by taking yet another time derivative of the evolution equation for the momentum variable. In that way, they are able to prescribe in a completely free way the lapseshift pair. In doing this, they obtain a nonstrictly hyperbolic system, in the sense of LerayOhya, [55], which I presume in the language of first order systems means that it is a weakly hyperbolic, but with certain other properties which imply that the system is well posed in Gevrey classes of functions ^{9}. The resulting system, once brought to first order, has a rather big number of variables. It is not clear that one can stablish numerical stability and convergence for these types of systems, for at least in the continuum estimates an infinite number of derivatives are involved.
In [32], as said in the previous section, a system in the frame representation is made where the corresponding gauge variables can also be given arbitrarily. The importance of this freedom is that in this case one can prescribe directly the lapse. This is in contrast to the case of the generalized harmonic time condition, in which one prescribes the lapse up to the square root of the metric and so finds out what the lapse really was only after solving the problem.
5.2 Hyperbolic Extensions
One would also like to have recipes which could be used automatically during evolution, that is, algebraic or differential equations, which would not only fix uniquely the evolution of the gauge variables, but which would also result in a well posed evolutionary problem.
Note that the above prescription for the evolution of the lapse for f = f_{0} > 0 is identical to the one considered in [35], namely equation 8. It is most probably the case then that the same sort of instability would be present there, although the equations considered there are different, due to the inclusion of terms proportional to the scalar constraint in order to render the system symmetric hyperbolic.
In [5] there is also a study of another type of singularity which is not ruled out with the choice of the harmonic gauge, f=1. This singularity seems to be of a different nature, and is probably related to the instability of the harmonic gauge already mentioned. It clearly has to do with the nonlinearities of the theory.
It should be mentioned that there are a wide variety of possibilities for making bigger hyperbolic systems out of those which are hyperbolic for a prescribed lapseshift pair, or for the generalized harmonic gauge variant. In that respect, perhaps the systems which are more amenable to a methodological and direct study are the ones in the frame or in Ashtekar’s representations, for there, as discussed in the previous section for the Ashtekar’s representation systems, § 4.3, the possibilities to enlarge the system and keep it symmetric hyperbolic are quite clear and limited.
5.3 Elliptic Extensions
These are other types of approaches which take more into account the longitudinal modes of the theory, namely those which are related to the energy or matter content of the space time, and those which do not propagate as waves. The nature of these modes implies that these approaches seem to need a global knowledge of the solution, which in practice appears by imposing either elliptic or parabolic equations, the latter as a way to drive the solution close to satisfying an elliptic equation for larger times. Systems of that sort have already been used in applications: In [23], a hyperbolic system with lapse given by an elliptic equation is used in the proof of global existence of small data. The elliptic equation is used to impose the maximal slice condition during evolution, that is P = 0. In that work, the first order system is for the electric and magnetic parts of the Weyl tensor, while the metric, connection, and extrinsic curvature tensor are obtained by solving elliptic equations on each slice. For their aims, obtaining a priori estimates, this suffices. For numerical simulations of evolution, it is better to solve, as much as possible, evolution equations, and not elliptic ones. Thus for this aim, equations hopefully hyperbolic or at least parabolic should be added to evolve the above mentioned (lower order in derivatives) variables. This has improved recently in [22], and [3] with a slight generalization to [23] in admitting arbitrarily prescribed P’s. In particular, in [22] a complete proof of well posedness of mixed symmetric hyperbolicelliptic systems is given. Such a proof must be implicit somewhere in [23], and a general argument has been given in [34]. Surprisingly, such a result, which has a rather simple argument based on the standard elliptic and hyperbolic estimates, has not before had the clean proof it deserves. This gauge has been used to show existence of near Newtonian solutions by [56].
In [34] a different elliptic condition is imposed in order to study near Newtonian solutions. An elliptic system is considered for both lapse and shift. It is similar, but not equal, to the above gauge, for in this work a much stronger condition is required on the order of approach of relativistic solutions to the Newtonian limit. This implies globally controlling not only the lapse, but also the shift.
The last two works mentioned hint at some interplay between the problems of finding well behaving gauges for near Newtonian solutions and for long term evolution. The argument has been that, since in this gauge the principal part of the equations is well behaved near the singular Newtonian limit, and since the rest of the terms of the hyperbolic system go to zero on that limit, one expects for the time the solution exists to go to infinity as one approaches the Newtonian limit. Thus the gauge should be well behaved until then. I cite [43] for recent work on this and [44] for a well behaved system in asymptotically null slices amenable to study slow solutions near null infinity.
In the frame and in Ashtekar’s representations one could even consider first order elliptic (spinorial) equations to fix the gauge variables. In the frame representation one can even fix gauge variables via an algebraic condition.
6 The Role of the Constraints
In this section, I analyze the role the constraint equations play in these new formulations. I will start by analyzing how the equations were handled in the original proof of well posedness. Then I discuss what has been said recently and what has to be done in the future, both for theoretical considerations and for numerical work. In particular, I discuss the role of the constraints in the initialboundary value problem, a problem which has still to be fully solved, but which nevertheless is applied in most of the numerical simulations.
6.1 The Constraints in the Harmonic Gauge
In the harmonic gauge, the role of the constraint equations as such is hidden. This is because the constraint equations become evolution equations due to the gauge choice. Indeed, in the full harmonic gauge all components of the Einstein tensor become a big second order hyperbolic equation for the metric components. The need for the constraints to be satisfied at the initial surface enters the picture because it implies that the first time derivative of the gauge condition must vanish there in order to guarantee that the constraints vanish everywhere. Thus the question about the preservation of the constraint equations does not appear here. At most one can say it has been traded for the question of the gauge consistency.
6.2 The Constraints in the New Systems: Theoretical Considerations
In the new hyperbolic systems, where covariance is lost, one solves only for the evolution equations. Thus, the question of whether the constraint equations hold during evolution if they hold at the initial surface arises again. If the problem is about the evolution of the whole spacetime, or about evolution on the domain of dependence of some spacelike surface, then there is a good argument showing that the constraint equations would be satisfied as a consequence of the uniqueness of the system under consideration:
Assume initial data is given at some spacelike hypersurface which satisfies the constraints there. We use the new evolution system and get a solution in the domain of dependence of the system, (which, if gauges propagate at speeds greater than light, might be smaller than the domain given by the metric). But using the harmonic gauge I know that there is a solution to the Einstein equation on a maximally extended domain of dependence. If one can diffeomorphically transform metric corresponding to that solution into one satisfying the gauge used for the evolution with the new system, then, since it satisfies all the equations, including the constraints, it follows that it will also satisfy the equations of the new system. Uniqueness of solutions of the new system implies it must be the one found initially and so it also satisfies the constraints. Thus we see that no particular consideration for the constraint equations is needed.
6.3 The Constraints in the New Systems: Numerical Considerations
For numerical simulations, the role of the constraint equations is delicate: Since there are always numerical errors, although the vector field defined by Einstein’s equations in any of the above approaches is tangent to the constraint submanifold, we can only expect to be in the neighborhood of that submanifold. So, since one is effectively modifying the evolution equations outside the submanifold, that the vector field is tangent to it is not enough. For if that submanifold were unstable, it could very well be that a spurious numerical solutions could start growing during evolution and takes us completely away from it. This problem has been noticed by several people and has been considered in detail in [33]. There it is shown that, while in some evolution systems, the constraints themselves obey hyperbolic evolution equations, in others that is not the case so are presumably unstable.
It is not clear to me that the condition that the constraint system be well posed is the one needed for considering a system free of this problem. First because well posedness as such is not enough to guarantee the possibility of a numerical scheme: The system could be well posed but still depart exponentially from the constraint submanifold, thus making impossible any reliable calculation. So the nonprincipal part of the system must also be considered, and probably suitably modified in the neighborhood of the constraint submanifold. Second, since one is never solving, or simulating, the constraint evolution equations, that is, they play no role in the scheme, why should one consider them at all? I think the emphasis should be put on guaranteeing a numerical scheme without spurious solutions; because, as argued above, uniqueness should imply that the constraints are satisfied. Thus, what seems to be needed is a connection between well posedness, or rather no exponential departure from the constraint submanifold, and lack of spurious solutions on the numerical schema.
6.4 The Constraints in the InitialBoundary Value Problem
A completely different situation arises if one is considering an initialboundary value problem for Einstein’s equations. Although this problem has not been solved in its full generality for Einstein’s equations, it is clear that in order for the constraints to be satisfied during evolution, some of the boundary values have to be chosen in a special way. It is here that the type of equations the constraints satisfy is most important. In particular, if they also form a hyperbolic system, then a study of its principal part at the boundary would tell which conditions are needed to guarantee uniqueness of the solutions, in particular the trivial solution, and so which are the boundary conditions we must force upon the evolution system for the dynamical fields. Since most numerical simulations are in fact initialboundary value problems, the problem of well posedness and the problem of the propagation of the constraints are central.
Footnotes
 1.
In this work, the linearized Einstein equations in terms of the conformal metric in a neighborhood of J were regularized and made hyperbolic. Thus local existence results applied to these equations showed that perturbations with smooth initial data at a hypersurface reaching J stayed bounded during evolution, and so the asymptotic structure was preserved to the future of that hypersurface.
 2.
Actually, for the machinery of proving well posedness, finite differentiability to some higher order is needed.
 3.
Extra conditions have to be imposed, like entropy growth across shocks, to obtain uniqueness.
 4.
That is, sufficiently smooth for the Sobolev energy, with minimum differentiability possible to close the bounds, to exist.
 5.
One could of course put a discontinuity on the derivatives of the metric on initial data. The discontinuity would propagate along the characteristics. In general this is not considered a shock, for it is not generated by the dynamics and does not propagate along a different characteristic than the neighboring continuous regions. These are called contact discontinuities.
 6.
If matter sources are included, like fluids, then one might need to consider flux conservative schema for the whole system of equations. But probably it would be much better to use relativistic dissipative fluids whose global existence for small data has been proven recently [52] to dispense of shocks altogether when considering weak data.
 7.If ε_{abcd} is the LeviCivita tensor corresponding to the physical metric, g^{ab} and ̃ε_{abcd} the one corresponding to background metric, ̃g^{ab}, then.$${\varepsilon _{abcd}}\; = \sqrt g {\tilde \varepsilon _{abcd}}$$
 8.
Note that the lapse used in this work already had the generalized harmonic time gauge built into it.
 9.
Basically one is able to bound norms on the solution by different norms on the initial data, with the last one involving more derivatives, but with smaller and smaller derivatives as the order of the derivatives in the norms increases.
References
 [1]Abrahams, A., Anderson, A., ChoquetBruhat, Y., and York Jr., J.W., “Hyperbolic formulation of general relativity”, (March, 1997), [Online Los Alamos Archive Preprint]: cited on 18 January 1998, http://xxx.lanl. gov/abs/grqc/9703010. 4.1Google Scholar
 [2]Abrahams, A., Anderson, A., ChoquetBruhat, Y., and York Jr., J.W., “Einstein and YangMills theories in hyperbolic form without gauge fixing”, Phys. Rev. Lett., 75, 3377–3381, (1995). For a related online version see: A. Abrahams, et al., “Einstein and YangMills theories in hyperbolic form without gauge fixing”, (June, 1995), [Online Los Alamos Archive Preprint]: cited on 19 January 1998, http://xxx.lanl.gov/abs/grqc/9506072. 4.1ADSMathSciNetCrossRefGoogle Scholar
 [3]Abrahams, A., Anderson, A., ChoquetBruhat, Y., and York Jr., J.W., “A nonstrictly hyperbolic system for the Einstein equations with arbitrary lapse and shift”, C. R. Acad. Sci., 323(serie IIb), 835–841, (1996). For a related online version see: A. Abrahams, et al., “A nonstrictly hyperbolic system for the Einstein equations with arbitrary lapse and shift”, (July, 1996), [Online Los Alamos Archive Preprint]: cited on 17 January 1998, http://xxx.lanl.gov/abs/grqc/9607006. 5.1, 5.3zbMATHGoogle Scholar
 [4]Abrahams, A., Anderson, A., ChoquetBruhat, Y., and York Jr., J.W., “Geometrical hyperbolic systems for general relativity and gauge”, Class. Quantum Grav., 14, A9–A22, (1997). For a related online version see: A. Abrahams, et al., “Geometrical hyperbolic systems for general relativity and gauge”, (May, 1996), [Online Los Alamos Archive Preprint]: cited on 16 April 1997, http://xxx.lanl.gov/abs/grqc/9605014. 4.1ADSMathSciNetCrossRefGoogle Scholar
 [5]Alcubierre, M., “Appearance of coordinate shocks in hyperbolic formalisms of general relativity”, Phys. Rev. D, 55, 5981–5991, (1997). 5, 7, 5.1, 5.2ADSMathSciNetCrossRefGoogle Scholar
 [6]Alcubierre, M., and Masso, J., “Pathologies of hyperbolic gauges in general relativity and other field theories”, (September, 1997), [Online Los Alamos Archive Preprint]: cited on 17 January 1998, http://xxx.lanl.gov/abs/grqc/9709024. 5.2
 [7]Ashtekar, A., “New Hamiltonian formulation of general relativity”, Phys. Rev. D, 36(6), 1587–1602, (1987). 4.3ADSMathSciNetCrossRefGoogle Scholar
 [8]Ashtekar, A., New Perspectives in Canonical Gravity, (Bibliopolis, Napoli, 1988). 4.3zbMATHGoogle Scholar
 [9]Bona, C., and Massó, J., “Hyperbolic evolution system for numerical relativity”, Phys. Rev. Lett., 68, 1097–1099, (1992). 4.1ADSMathSciNetCrossRefGoogle Scholar
 [10]Bona, C., Massó, J., Seidel, E., and Stela, J., “First order hyperbolic formalism for Numerical Relativity”, (September, 1997), [Online Los Alamos Archive Preprint]: cited on 19 January 1998, http://xxx.lanl.gov/abs/grqc/9709016. 4.1, 4.3, 5.2ADSMathSciNetCrossRefGoogle Scholar
 [11]Bona, C., Massó, J., Seidel, E., and Stela, J., “New Formalism for Numerical Relativity”, Phys. Rev. Lett., 75, 600–603, (1995). For a related online version see: C. Bona, et al., “New formalism for numerical relativity”, (December, 1994), [Online Los Alamos Archive Preprint]: cited on 19 January 1998, http://xxx.lanl.gov/abs/grqc/9412071. 4.1,5.2ADSCrossRefGoogle Scholar
 [12]Bona, C., Massó, J., and Stela, J., “Numerical black holes: a moving grid approach”, Phys. Rev. D, 51, 1639–1645, (1995). For a related online version see: C. Bona, et al., “Numerical black holes: a moving grid approach”, (December, 1994), [Online Los Alamos Archive Preprint]: cited on 19 January 1998, http://xxx.lanl.gov/abs/grqc/9412070. 5.2ADSCrossRefGoogle Scholar
 [13]Bruhat, Y., “Theoreme d’ existence pour certain systemes d’equations aux derivees partielles nonlinaires”, Acta Math., 88, 141–225, (1952). 1.1ADSMathSciNetCrossRefGoogle Scholar
 [14]Bruhat, Y., “Un theoreme d’inestabilite pour certain equations hyperboliques nonlinaires”, C. R. Acad. Sci., 276A, 281, (1973). 7, 5.1Google Scholar
 [15]ChoquetBruhat, Y., “The Cauchy Problem”, in Witten, L., ed., Gravitation: an introduction to current research, 68–103, (Wiley, New York, USA, 1962).Google Scholar
 [16]ChoquetBruhat, Y., “Espaces temps eineiniens généraux, chocs gravitationnels”, Ann. Inst. Henri Poincare, 8, 327–338, (1968). 1.1ADSzbMATHGoogle Scholar
 [17]ChoquetBruhat, Y., and Christodoulou, D., “Elliptic systems in H_{sg} spaces on manifolds which are Euclidean at infinity”, Acta Math., 145, 129–150, (1981). 1.1CrossRefGoogle Scholar
 [18]ChoquetBruhat, Y., Christodoulou, D., and Francaviglia, M., “Cauchy data on a manifold”, Ann. Inst. Henri Poincare, A, 29, 241–255, (1978). 1.1, 3ADSMathSciNetzbMATHGoogle Scholar
 [19]ChoquetBruhat, Y., and Ruggeri, T., “Hyperbolicity of the 3+1 System of Einstein Equations”, Commun. Math. Phys., 89, 269–275, (1983). 4.1, 8, 5.2ADSMathSciNetCrossRefGoogle Scholar
 [20]ChoquetBruhat, Y., and York Jr., J.W., “The Cauchy Problem”, in Held, A., ed., General Relativity and Gravitation 1, (Plenum, New York, USA, 1980).Google Scholar
 [21]ChoquetBruhat, Y., and York Jr., J.W., “Well posed reduced systems for the Einstein equations”, Comptes Ren. Acad. Paris, 231(I), 10891095, (1995). For a related online version see: Y. ChoquetBruhat, et al., “Well posed reduced systems for the Einstein equations”, (June, 1996), [Online Los Alamos Archive Preprint]: cited on 19 January 1998, http://xxx.lanl.gov/abs/grqc/9606001.
 [22]ChoquetBruhat, Y., and York Jr., J.W., “Mixed elliptic and hyperbolic system for the Einstein equations”. Editions Pitagora, (1996). For a related online version see: Y. ChoquetBruhat, et al., “Mixed elliptic and hyperbolic system for the Einstein equations”, (January, 1996), [Online Los Alamos Archive Preprint]: cited on 17 January 1998, http://xxx.lanl.gov/abs/grqc/9601030. 5.3
 [23]Christodoulou, D., and Klainerman, S., The Global Nonlinear Stability of the Minkowski Space, (Princeton University Press, Princeton, USA, 1993). 1, 3, 5.3zbMATHGoogle Scholar
 [24]Christodoulou, D., and O’Murchadha, N., “The Boost Problem in General Relativity”, Commun. Math. Phys., 80, 271–300, (1981). 1.1ADSMathSciNetCrossRefGoogle Scholar
 [25]Cutler, C., and Wald, R., “Existence of radiating EinteinMaxwell solutions which are C∞ on all of J^{+} and J^{}”, Class. Quantum Grav., 6, 453–466, (1989). 1ADSCrossRefGoogle Scholar
 [26]DeTurk, D., “The Cauchy problem for Lorentz metrics with prescribed Ricci curvature”, Comp. Math., 48, 327–349, (1983). 3.1ADSMathSciNetGoogle Scholar
 [27]Fischer, A., and Marsden, J., “The Einstein Evolution Equations as a FirstOrder Symmetric Hyperbolic Quasilinear System”, Commun. Math. Phys., 28, 1–38, (1972). 1.1ADSCrossRefGoogle Scholar
 [28]Fischer, A. Marsden, J., “General relativity, partial differential equations, and dynamical systems”, AMS Proc. Symp. Pure Math., 23, 309–327, (1973). 1.1MathSciNetCrossRefGoogle Scholar
 [29]Friedrich, H., “The asymptotic characteristic initial value problem for Einstein’s vacuum field equations as an initial value problem for a firstorder quasilinear symmetric hyperbolic system”, Proc. R. Soc. London, Ser. A, 378, 401–421, (1981). 1.1, 4.2ADSCrossRefGoogle Scholar
 [30]Friedrich, H., “On the regular and the asymptotic characteristic initial value problem for Einstein’s vacuum field equations”, Proc. R. Soc. London, Ser. A, 375, 169–184, (1981). 1.1, 4.2ADSMathSciNetCrossRefGoogle Scholar
 [31]Friedrich, H., “On the hyperbolicity of Einstein’s and other gauge field equations”, Commun. Math. Phys., 100, 525–543, (1985). 7, 4.2ADSMathSciNetCrossRefGoogle Scholar
 [32]Friedrich, H., “Hyperbolic reductions for Einstein’s equations”, Class. Quantum Grav., 13, 1451–1469, (1996). 1.2, 3, 7, 8, 4.2, 9ADSMathSciNetCrossRefGoogle Scholar
 [33]Frittelli, S., “Note on the propagation of the constraints in standard 3+1 general relativity”, Phys. Rev. D, 55, 5992–5996, (1997). 3.2, 6.3ADSMathSciNetCrossRefGoogle Scholar
 [34]Frittelli, S., and Reula, O., “On the newtonian limit of general relativity”, Commun. Math. Phys., 166, 221–235, (1994). For a related online version see: S. Frittelli, et al., “On the Newtoninan limit of general relativity”, (June, 1995), [Online Los Alamos Archive Preprint]: cited on 19 January 1998, http://xxx.lanl.gov/abs/grqc/9506077. 4.1,4.3,5.3ADSMathSciNetCrossRefGoogle Scholar
 [35]Frittelli, S., and Reula, O., “Firstorder symmetrichyperbolic Einstein equations with arbitrary fixed gauge”, Phys. Rev. Lett., 76, 4667–4670, (1996). For a related online version see: S. Frittelli, et al., “Firstorder symmetrichyperbolic Einstein equations with arbitrary fixed gauge”, (May, 1996), [Online Los Alamos Archive Preprint]: cited on 17 January 1998, http://xxx.lanl.gov/abs/grqc/9605005. 8, 5.2ADSCrossRefGoogle Scholar
 [36]Geroch, R., “Partial Differential Equations of Physics”, (February, 1996), [Online Los Alamos Archive Preprint]: cited on 19 January 1998, http://xxx.lanl.gov/abs/grqc/9602055. Scottish Summer School in Theoretical Physics. 1.2, 6, 3Google Scholar
 [37]Geroch, R., “The Local Nonsingularity Theorem”, J. Math. Phys., 24(7), 1851–1858, (1983). 1.1ADSMathSciNetCrossRefGoogle Scholar
 [38]Geroch, R., and Xanthopolous, B. C., “Asymptotic Simplicity Is Stable”, J. Math. Phys., 19, 714–719, (1978). 1ADSMathSciNetCrossRefGoogle Scholar
 [39]Gustaffson, B., Kreiss, H.O., and Oliger, J., TimeDependent Problems and Difference Methods, (Wiley, New York, USA, 1995). 1.2, 2, 2.4, 6zbMATHGoogle Scholar
 [40]Hadamard, J., Lectures on Cauchy’s problem in linear partial differential equations, (Yale University Press, New Haven, Connecticut, 1921). 2.1zbMATHGoogle Scholar
 [41]Hawking, S.W., and Ellis, G.F.R., The Large Scale Structure of SpaceTime, (Cambridge University Press, Cambridge, United Kingdom, 1973). 2, 3.1, 7CrossRefGoogle Scholar
 [42]Hughes, T., Kato, T., and Marsden, J., “Wellposed quasilinear second order hyperbolic systems with applications to nonlinear elastodynamics and general relativity”, Arch. Rat. Mech. Anal., 63, 273–294, (1976). 1.1, 3MathSciNetCrossRefGoogle Scholar
 [43]Iriondo, M., Leguizamón, E., and Reula, O., “Fast and Slow Solutions in General Relativity: The Initialization Procedure”, (September, 1997), [Online Los Alamos Archive Preprint]: cited on 17 January 1998, http://xxx.lanl.gov/abs/grqc/9709078. 5.3
 [44]Iriondo, M., Leguizamón, E., and Reula, O., “The Newtonian Limit on Asymptotically Null Foliations”, (September, 1997), [Online Los Alamos Archive Preprint]: cited on 17 January 1998, http://xxx.lanl.gov/grqc/970907. 5.3
 [45]Iriondo, M., Leguizamón, E., and Reula, O., “Einstein’s equations in Ashtekar variables constitute a symmetric hyperbolic system”, Phys. Rev. Lett., 79, 4732–4735, (1997). For a related online version see: M. Iriondo, et al., “Einstein’s equations in Ashtekar variables constitute a symmetric hyperbolic system”, (October, 1997), [Online Los Alamos Archive Preprint]: cited on 17 January 1998, http://xxx.lanl.gov/abs/grqc/9710004. 4.3ADSCrossRefGoogle Scholar
 [46]John, F., Formation of Singularities in Elastic Waves. Lecture Notes in Phys., (SpringerVerlag, 1984). 2, 4, 4.2Google Scholar
 [47]Klainerman, S., “Uniform decay estimates and the Lorentz invariance of the classical wave equation”, Commun. Pure Appl. Math., 38, 321–332, (1985). 1ADSMathSciNetCrossRefGoogle Scholar
 [48]Klainerman, S., “The null condition and global existence to nonlinear wave equations”, Lect. Appl. Math., 23, 293–326, (1986). 1MathSciNetzbMATHGoogle Scholar
 [49]Klainerman, S., “Remarks on the global Sobolev inequalities in Minkowski Space”, Commun. Pure Appl. Math., 40, 111–117, (1987). 1MathSciNetCrossRefGoogle Scholar
 [50]Kreiss, H., and Lorentz, J., InitialBoundary Value Problems and the NavierStokes Equations, (Acad. Press, San Diego, USA, 1989). 1.2, 2, 6Google Scholar
 [51]Kreiss, H. O., “Über sachgemässe Cauchyprobleme”, Math. Scand., 7, 71–80, (1959). 2MathSciNetCrossRefGoogle Scholar
 [52]Kreiss, H.O., Nagy, G., Ortiz, O., and Reula, O., “Global Existence and Exponential Decay for Hyperbolic Dissipative Relativistic Fluid Theories”, J. Math. Phys., 38, 5272–5279, (1997). For a related online version see: H.O. Kreiss, et al., “Global Existence and Exponential Decay for Hyperbolic Dissipative Relativistic Fluid Theories”, (February, 1997), [Online Los Alamos Archive Preprint]: cited on 19 January 1998, http://xxx.lanl.gov/abs/grqc/9702008. 6ADSMathSciNetCrossRefGoogle Scholar
 [53]Lanczos, C., “Ein vereinfachendes Koordinatensystem fur die Einsteinschen Gravitationsgleichungen”, Phys. Z., 23, 537–539, (1922).zbMATHGoogle Scholar
 [54]Leray, J., Hyperbolic Differential Equations, (Institute for Advanced Studies, Princeton, New Jersey, 1953). 2.1, 2.2Google Scholar
 [55]Leray, J., and Ohya, Y., “Equations et Systemes NonLineaires hyperboliques nonstricts”, Math. Ann., 170, 167, (1967). 2.1, 2.2, 5.1MathSciNetCrossRefGoogle Scholar
 [56]Rendall, A., “The Newtonian limit for asymptotically flat solutions of the VlasovEinstein system”, Commun. Math. Phys., 163, 89–112, (1994). For a related online version see: A. Rendall, “The Newtonian limit for asymptotically flat solutions of the VlasovEinstein system”, (March, 1993), [Online Los Alamos Archive Preprint]: cited on 7 January 1998, http://xxx.lanl.gov/abs/grqc/9303027. 5.3ADSMathSciNetCrossRefGoogle Scholar
 [57]Sideris, T., “Formation of Singularities in 3d Compressible Fluids”, Commun. Math. Phys., 101, 475–485, (1985). 2, 4ADSMathSciNetCrossRefGoogle Scholar
 [58]Taylor, M., Pseudodifferential operators and nonlinear PDE — Progress in Mathematics 100, (Birkhauser, Boston, USA, 1991). 3, 3, 6CrossRefGoogle Scholar
 [59]van Putten, M.H.P.M., and Eardley, D.M., “Nonlinear wave equations for relativity”, Phys. Rev. D, 53, 3056–3063, (1996). For a related online version see: M.H.P.M. van Putten, et al., “Nonlinear wave equations for relativity”, (May, 1995), [Online Los Alamos Archive Preprint]: cited on 17 January 1998, http://xxx.lanl.gov/abs/grqc/9505023. 4.2ADSMathSciNetCrossRefGoogle Scholar
 [60]Wald, R., General Relativity, (The University of Chicago Press, Chicago, USA, 1984). 2CrossRefGoogle Scholar
Copyright information
This article is distributed under the terms of the Creative Commons Attribution 4.0 International License (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted use, distribution, and reproduction in any medium, provided you give appropriate credit to the original author(s) and the source, provide a link to the Creative Commons license, and indicate if changes were made.