# Initial value formulation (general relativity)

The

**initial value formulation**is a way of expressing the formalism of Einstein's theory ofgeneral relativity in a way that describes auniverse evolving overtime .Each solution of Einstein's equation encompasses the whole history of a universe – it is not just some snapshot of how things are, but a whole

spacetime : a statement encompassing the state of matter and geometry everywhere and at every moment in that particular universe. By this token, Einstein's theory appears to be different from most other physical theories, which specifyevolution equation s for physical systems; if the system is in a given state at some given moment, the laws of physics allow you to extrapolate its past or future. For Einstein's equations, there appear to be subtle differences compared with other fields: they are self-interacting (that is,non-linear even in the absence of other fields; they are diffeomorphism invariant, so two obtain a unique solution, a fixed background metric and gauge conditions need to be introduced; finally, the metric determines the spacetime structure, and thus the domain of dependence for any set of initial data, so the region on which a specific solution will be defined is not, a priori, defined. [*Cf. Harvnb|Hawking|Ellis|1973|loc=sec. 7.1.*]There is, however, a way to re-formulate Einstein's equations that overcomes these problems. First of all, there are ways of re-writing spacetime as the evolution of "space" in time; an earlier version of this is due to

Paul Dirac , while a simpler way is known after its inventors Arnowitt, Deser and Misner asADM formalism . In these formulations, also known as "3+1" approaches, spacetime is split into a three-dimensional hypersurface withinterior metric and an embedding into spacetime withexterior curvature ; these two quantities are the dynamical variables in aHamiltonian formulation tracing the hypersurface's evolution over time. [*Harvnb|Arnowitt|Deser|Misner|1962; for a pedagogical introduction, see Harvnb|Misner|Thorne|Wheeler|1973|loc=§21.4–§21.7.*] With such a split, it is possible to state the*initial value formulation of general relativity*. It involves initial data which cannot be specified arbitrarily but needs to satisfy specificconstraint equations, and which is defined on some suitably smooth three-manifold $Sigma$; just as for other differential equations, it is then possible to prove existence and uniqueness theorems, namely that there exists a unique spacetime which is a solution of Einstein equations, which is globallyhyperbolic , for which $Sigma$ is aCauchy surface (i.e. all past events influence what happens on $Sigma$, and all future events are influenced by what happens on it), and has the specified internal metric and extrinsic curvature; all spacetimes that satisfy these conditions are related by isometries. [*Harvnb|Fourès-Bruhat|1952 and Harvnb|Bruhat|1962; for a pedagogical introduction, see Harvnb|Wald|1984|loc=ch. 10; an online review can be found in Harvnb|Reula|1998.*]The initial value formulation with its 3+1 split is the basis of

numerical relativity ; attempts to simulate the evolution of relativistic spacetimes (notably merging black holes or gravitational collapse) using computers. [*See Harvnb|Gourgoulhon|2007.*] However, there are significant differences to the simulation of other physical evolution equations which make numerical relativity especially challenging, notably the fact that the dynamical objects that are evolving include space and time itself (so there is no fixed background against which to evaluate, for instance, perturbations representing gravitational waves) and the occurrence of singularities (which, when they are allowed to occur within the simulated portion of spacetime, lead to arbitrarily large numbers that would have to be represented in the computer model). [*For a review of the basics of numerical relativity, including the problems alluded to here and further difficulties, see Harvnb|Lehner|2001.*]**ee also***

Einstein's equations

*ADM formalism **Notes****References***Arnowitt, Richard

; Stanley Deser& Charles W. Misner(1962),"The dynamics of general relativity", inWitten, L.,"Gravitation: An Introduction to Current Research", Wiley, pp. 227-265

*Bruhat, Yvonne(1962),"The Cauchy Problem", inWitten, Louis,"Gravitation: An Introduction to Current Research", Wiley, pp. 130

*Citation

first=Yvonne

last= Fourès-Bruhat

title= Théoréme d'existence pour certains systémes d'équations aux derivées partielles non linéaires

journal= Acta Mathematica

volume=88

year=1952

pages=141–225

*Citation

first=Eric

last=Gourgoulhon

title=3+1 Formalism and Bases of Numerical Relativity

id=arxiv|gr-qc|0703035

year=2007

*Citation

last1=Hawking

first1=Stephen W.

last2=Ellis

first2=George F. R.

title=The large scale structure of space-time

publisher=Cambridge University Press

isbn=0-521-09906-4

year=1973

*Citation

last=Lehner

first=Luis

title=Numerical Relativity: A review

journal =Class. Quant. Grav.

volume=18

year=2001

pages=R25-R86

id=arxiv|gr-qc|0106072

* Misner, Charles W.; Kip. S. Thorne& John A. Wheeler(1973),"Gravitation", W. H. Freeman, ISBN 0-7167-0344-0

*Citation

first= Oscar A.

last=Reula

title=Hyperbolic Methods for Einstein's Equations

journal=Living Rev. Relativity

volume=1

year=1998

url=http://www.livingreviews.org/lrr-1998-3

accessdate=2007-08-29

* Wald, Robert M.(1984),""General Relativity"", Chicago: University of Chicago Press, ISBN 0-226-87033-2

*Wikimedia Foundation.
2010.*

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