Einstein's GR field equationsEinsteinsGRFieldEquations2009-01-27 11:49:112009-01-27 12:49:00TopicGR field equationsGeneral Relativiy field equationsGR field equationsGeneral Relativiy field equationsAlbert Einstein's GR equationsQuantumRiemannianGeometryalternative formulations of GR field equations and GRAQFTHaag's Local Quantum Physics\section{Introduction}
The following is a brief presentation cited from a \PMlinkexternal{PM entry reference on Einstein's Field Equations.}{http://planetmath.org/?op=getobj&from=objects&name=EinsteinFieldEquations}
The interested reader may click on the above link to see the complete reference
cited here which provides additional mathematical data/information.
\subsection{Einstein's Field Equations in General Relativity}
``{\em Then the Einstein equations read as follows:
``
\footnote{In the physics literature, the coefficient of $T_{\mu \nu}$ is
written as $\frac{8\pi G}{c^4}$, where $G$ is the gravitational constant,
$c$ is the light velocity constant but, since we are interested in the purely
mathematical properties of these equations, we shall set $G = c = 1$ here,
which may be accomplished by working in a suitable set of physical units.
It might also be worth mentioning that, in physics, the tensor $T_{\mu \nu}$
is the stress-energy tensor, which encodes data pertaining to the mass, energy, and momentum densities of the surrounding space. The number $\Lambda$
is known as the cosmological constant because it determines large-scale
properties of the universe, such as whether it collapses, remains stationary, or expands.''}
\[G_{\mu \nu} = \Lambda g_{\mu \nu} + 8 \pi T_{\mu \nu}\]
Here, $G_{\mu\upsilon}=R_{\mu\upsilon}-\frac{1}{2}g_{\mu\upsilon}R$
is the \emph{Einstein Tensor}, $R_{\mu\upsilon}$ is the Ricci tensor, and
$R=g^{\mu\nu}R_{\mu\nu}$ is the Ricci scalar, and $g^{\mu\nu}$ is the
inverse metric tensor.}
{\em One possibility is that the tensor field $T_{\mu \nu}$ is specified and that these equations are then solved to obtain $g_{\mu \nu}$. A noteworthy case of this is the \emph{vacuum Einstein equations}, in which
$$T_{\mu \nu} = 0.$$
Another possibility is that $T_{\mu \nu}$ is given in terms of some other fields on the manifold and that the Einstein equations are augmented by differential equations which describe those fields. In that case, one speaks of Einstein-Maxwell equations, Einstein-Yang-Mills equations, and the like depending on what these other fields may happen to be. It should be noted that, on account of the Bianchi identity, there is an integrability condition $\nabla_\mu (g) T^{\mu \nu} = 0$. (Here, $\nabla (g)$ denotes covariant differentiation with respect to the Levi-Civita connection of the metric tensor $g_{\mu \nu}$).
When choosing $T_{\mu \nu}$, these conditions must be taken into account in order to guarantee that a solution is possible.}''
\section{Alternative Formulations of GR field equations and General Relativity theories}
An alternative, more general formulation would involve a categorical framework
such as the category of pseudo-Riemannian manifolds, and/or the category of Riemannian manifolds,
with, or without, a Riemannian metric. Expanding universes and black hole singularities,
with or without hair, either with an event horizon, or `naked' can be treated within
such an unified categorical framework of Riemannian/ pseudo-Riemanian manifolds and their
transformations represented either as morphisms or by functors and natural transformations
between functors. Quantized versions in quantum gravity may also be available based on
spin foams represented by time-dependent/ parameterized functors between spin networks
including extremely intense, but finite, gravitational fields. A Quantum Riemannian Geometry, that is, a quantized `Riemannian--like' manifold has also been reported in attempts to formulate a Quantum Gravity theory based on a \PMlinkname{quantized (or deformed)non-commutative `Riemannian manifold'}{ QuantumRiemannianGeometry}.
An alternative approach has already been reported recently as `Local Quantum Physics' by Haag and others, or in a more general setting as ``Algebraic (or `Axiomatic') Quantum Field Theory'' (AQFT).
\section{Conjectures}
\subsection{The Penrose Conjecture}
Sir Roger Penrose formulated sometime ago an important conjecture
regarding physical black holes:
``{\em All physical black holes have an event horizon; naked black holes are physically prohibited or forbidden even though they may be mathematically possible.}''
John Wheeler also formulated a conjecture related to the above:
``{\em All black holes are `without hair' (are completely invisible as no radiation escapes any black hole.''}
Stephen William Hawking and others seem to have proven theoretically and decisively that black holes have `hair', that is, that they can radiate
what is now called `Hawking' radiation. Thus the J. Wheerle conjecture seems to be incorrect. Furthermore, recent astrophysical theories and observations seem
to disprove also the `Penrose conjecture', and suggest the existence of naked
nlack holes without an event horizon, thus going much further than the Hawking's model of black holes `with hair'.
\section{Hyperbolic Formulations}
\section{Variational Principles}
\section{Global Structure}
\section{Initial Value Formulation}
\section{Special Solutions}
\subsubsection{Spatially Homogeneous Solutions}
\subsubsection{Solutions with Symmetries}
\subsubsection{Algebraically Special Solutions}
\subsubsection{Linearization}
\subsubsection{Singularities}
\subsubsection{Asymptotically Flat Solutions}
\subsubsection{Existence Theorems}