ADM mass
$G\_\{\backslash mu\; \backslash nu\}\; +\; \backslash Lambda\; g\_\{\backslash mu\; \backslash nu\}=\; \{8\backslash pi\; G\backslash over\; c^4\}\; T\_\{\backslash mu\; \backslash nu\}$ 

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The ADM formalism developed in 1959 by Richard Arnowitt, Stanley Deser and Charles W. Misner is a Hamiltonian formulation of general relativity. This formulation plays an important role both in quantum gravity and numerical relativity.^{[2]}
A comprehensive review of this formalism was published by the same authors in Gravitation: An introduction to current research Louis Witten (editor), Wiley NY (1962); chapter 7, pp 227–265. Recently, this has been reprinted in the journal General Relativity and Gravitation.^{[3]} The original papers can be found in Physical Review archives.^{[2]}^{[4]}^{[5]}^{[6]}^{[7]}^{[8]}^{[9]}^{[10]}^{[11]}
Contents
Overview
The formalism supposes that spacetime is foliated into a family of spacelike surfaces $\backslash Sigma\_t$, labeled by their time coordinate $t$, and with coordinates on each slice given by $x^i$. The dynamic variables of this theory are taken to be the metric tensor of three dimensional spatial slices $\backslash gamma\_\{ij\}(t,x^k)$ and their conjugate momenta $\backslash pi^\{ij\}(t,x^k)$. Using these variables it is possible to define a Hamiltonian, and thereby write the equations of motion for general relativity in the form of Hamilton's equations.
In addition to the twelve variables $\backslash gamma\_\{ij\}$ and $\backslash pi^\{ij\}$, there are four Lagrange multipliers: the lapse function, $N$, and components of shift vector field, $N\_i$. These describe how each of the "leaves" $\backslash Sigma\_t$ of the foliation of spacetime are welded together. The equations of motion for these variables can be freely specified; this freedom corresponds to the freedom to specify how to lay out the coordinate system in space and time.
Derivation
Notation
Most references adopt notation in which four dimensional tensors are written in abstract index notation, and that Greek indices are spacetime indices taking values (0, 1, 2, 3) and Latin indices are spatial indices taking values (1, 2, 3). In the derivation here, a superscript (4) is prepended to quantities that typically have both a threedimensional and a fourdimensional version, such as the metric tensor for threedimensional slices $g\_\{ij\}$ and the metric tensor for the full fourdimensional spacetime $\{^\{(4)\}\}g\_\{\backslash mu\; \backslash nu\}$.
The text here uses Einstein notation in which summation over repeated indices is assumed.
Two types of derivatives are used: Partial derivatives are denoted either by the operator $\backslash partial\_\{i\}$ or by subscripts preceded by a comma. Covariant derivatives are denoted either by the operator $\backslash nabla\_\{i\}$ or by subscripts preceded by a semicolon.
The determinant of the metric tensor is represented by $g$ (with no indices). Other tensor symbols written without indices represent the trace of the corresponding tensor such as $\backslash pi\; =\; g^\{ij\}\backslash pi\_\{ij\}$.
Lagrangian Formulation
The starting point for the ADM formulation is the Lagrangian
 $\backslash mathcal\{L\}\; =\; \{^\{(4)\}R\}\; \backslash sqrt\{^\{(4)\}g\}$
which is a product of the square root of the determinant of the fourdimensional metric tensor for the full spacetime and its Ricci scalar. This is the Lagrangian from the EinsteinHilbert action.
The desired outcome of the derivation is to define an embedding of threedimensional spatial slices in the fourdimensional spacetime. The metric of the threedimensional slices
 $g\_\{ij\}\; =\; \{^\{(4)\}\}g\_\{ij\}\backslash ,\backslash !$
will be the generalized coordinates for a Hamiltonian formulation. The conjugate momenta can then be computed
 $\backslash pi^\{ij\}\; =\; \backslash sqrt\{^\{(4)\}g\}\; \backslash left(\; \{^\{(4)\}\}\backslash Gamma^\{0\}\_\{pq\}\; \; g\_\{pq\}\; \{^\{(4)\}\}\backslash Gamma^\{0\}\_\{rs\}g^\{rs\}\; \backslash right)\; g^\{ip\}g^\{jq\}$
using standard techniques and definitions. The symbols $\{^\{(4)\}\}\backslash Gamma^0\_\{ij\}$ are Christoffel symbols associated with the metric of the full fourdimensional spacetime. The lapse
 $N\; =\; \backslash left(\; \{^\{(4)\}g\_\{00\}\}\; \backslash right)\; ^\{1/2\}$
and the shift vector
 $N\_\{i\}\; =\; \{^\{(4)\}g\_\{0i\}\}\backslash ,\backslash !$
are the remaining elements of the fourmetric tensor.
Having identified the quantities for the formulation, the next step is to rewrite the Lagrangian in terms of these variables. The new expression for the Lagrangian
 $\backslash mathcal\{L\}\; =\; g\_\{ij\}\; \backslash partial\_\{t\}\; \backslash pi^\{ij\}\; \; NH\; \; N\_\{i\}P^\{i\}\; \; 2\; \backslash partial\_\{i\}\; (\; \backslash pi^\{ij\}\; N\_\{j\}\; \; \backslash frac\{1\}\{2\}\; \backslash pi\; N^\{i\}\; +\; \backslash nabla^\{i\}\; N\; \backslash sqrt\{g\}\; )$
is conveniently written in terms of the two new quantities
 $H\; =\; \backslash sqrt\{g\}\; \backslash left[\; R\; +\; g^\{1\}\backslash left(\backslash frac\{1\}\{2\}\; \backslash pi^\{2\}\; \; \backslash pi^\{ij\}\backslash pi\_\{ij\}\; \backslash right)\; \backslash right]$
and
 $P^\{i\}\; =\; 2\; \backslash pi^\{ij\}\{\}\_\{;j\}$
which are known as the Hamiltonian constraint and the momentum constraint respectively. Note also that the lapse and the shift appear in the Hamiltonian as Lagrange multipliers.
Equations of Motion
Although the variables in the Lagrangian represent the metric tensor on threedimensional spaces embedded in the fourdimensional spacetime, it is possible and desirable to use the usual procedures from Lagrangian mechanics to derive "equations of motion" that describe the time evolution of both the metric $g\_\{ij\}$ and its conjugate momentum $\backslash pi^\{ij\}$. The result
 $\backslash partial\_\{t\}\; g\_\{ij\}\; =\; 2Ng^\{1/2\}\; (\; \backslash pi\_\{ij\}\; \; \backslash frac\{1\}\{2\}\; \backslash pi\; g\_\{ij\}\; )\; +\; N\_\{i;j\}\; +\; N\_\{j;i\}$
and
 $\backslash partial\_\{t\}\; \backslash pi^\{ij\}\; =\; N\backslash sqrt\{g\}\; (\; R^\{ij\}\; \; \backslash frac\{1\}\{2\}\; R\; g^\{ij\}\; )\; +\; \backslash frac\{1\}\{2\}\; Ng^\{1/2\}g^\{ij\}\; (\; \backslash pi^\{mn\}\backslash pi\_\{mn\}\; \; \backslash frac\{1\}\{2\}\; \backslash pi^\{2\}\; )\; \; 2Ng^\{1/2\}\; (\; \backslash pi^\{in\}\backslash pi\_\{n\}\{\}^\{j\}\; \; \backslash frac\{1\}\{2\}\backslash pi\backslash pi^\{ij\}\; )$
 $\backslash sqrt\{g\}(\backslash nabla^\{i\}\backslash nabla^\{j\}N\; g^\{ij\}\backslash nabla^\{n\}\backslash nabla\_\{n\}N)\; +\; \backslash nabla\_\{n\}(\; \backslash pi^\{ij\}N^\{n\}\; )\; \; N^\{i\}\{\}\_\{;n\}\backslash pi^\{nj\}\; \; N^\{j\}\{\}\_\{;n\}\backslash pi^\{ni\}$
is a nonlinear set of partial differential equations.
Taking variations with respect to the lapse and shift provide constraint equations
 $H\; =\; 0$
and
 $P^\{i\}\; =\; 0$
and the lapse and shift themselves can be freely specified, reflecting the fact that coordinate systems can be freely specified in both space and time.
Application to Quantum Gravity
Using the ADM formulation, it is possible to attempt to construct a quantum theory of gravity, in the same way that one constructs the Schrödinger equation corresponding to a given Hamiltonian in quantum mechanics. That is, replace the canonical momenta $\backslash pi^\{ij\}(t,x^k)$ and the spatial metric functions by linear functional differential operators
 $\backslash hat\{g\}\_\{ij\}(t,x^k)\; \backslash to\; g\_\{ij\}(t,x^k)$
 $\backslash hat\{\backslash pi\}^\{ij\}(t,x^k)\; \backslash to\; i\; \backslash frac\{\backslash delta\}\{\backslash delta\; g\_\{ij\}(t,x^k)\}$
More precisely, the replacing of classical variables by operators is restricted by commutation relations. The hats represents operators in quantum theory. This leads to the WheelerdeWitt equation.
Application to Numerical Solutions of the Einstein Equations
There are relatively few exact solutions to the Einstein field equations. In order to find other solutions, there is an active field of study known as numerical relativity in which supercomputers are used to find approximate solutions to the equations. In order to construct such solutions numerically, most researchers start with a formulation of the Einstein equations closely related to the ADM formulation. The most common approaches start with an initial value problem based on the ADM formalism.
In Hamiltonian formulations, the basic point is replacement of set of second order equations by another first order set of equations. We may get this second set of equations by Hamiltonian formulation in an easy way. Of course this is very useful for numerical physics, because the reduction of order of differential equations must be done, if we want to prepare equations for a computer.
ADM Energy
ADM energy is a special way to define the energy in general relativity which is only applicable to some special geometries of spacetime that asymptotically approach a welldefined metric tensor at infinity — for example a spacetime that asymptotically approaches Minkowski space. The ADM energy in these cases is defined as a function of the deviation of the metric tensor from its prescribed asymptotic form. In other words, the ADM energy is computed as the strength of the gravitational field at infinity.
The quantity is also called the ADM Hamiltonian, especially if one finds a different formula than the definition above that however leads to the same result.
If the required asymptotic form is timeindependent (such as the Minkowski space itself), then it respects the timetranslational symmetry. Noether's theorem then implies that the ADM energy is conserved. According to general relativity, the conservation law for the total energy does not hold in more general, timedependent backgrounds  for example, it is completely violated in physical cosmology. Cosmic inflation in particular is able to produce energy (and mass) from "nothing" because the vacuum energy density is roughly constant, but the volume of the Universe grows exponentially.
See also
 Canonical coordinates
 Canonical gravity
 Hamiltonian mechanics
 Hamilton–Jacobi–Einstein equation
 WheelerdeWitt equation
 Peres metric
References