General Relativity

1 Introduction

Einstein's General Relativity is a theory of gravity which is based on the Equivance Principle that asserts that a uniform gravitational field (next to an infinite flat massive body) is indistinguishable from a uniform accelleration.

$ \nabla \cdot \mathbf {A} =-4\pi G\rho $

2 Coordinate Systems

We will use the Einstein Notation. Consider Cartesian space in $ \mathbb {R} ^{2} $, covered by Cartisian coordinates $ (x^{1},x^{2})\, $. Pythagorous can be used to give the squared differential displacement:

$ ds^{2}=(dx^{1})^{2}+(dx^{2})^{2}\, $

Now consider a general curvilinear coordinate system (CS) $ (y^{1},y^{2}\,) $. Since the lines of the CS are neither parallel nor perpendicular, we form the same quantity:

$ ds^{2}=g_{11}(dy^{1})^{2}+2g_{12}dx^{1}dx^{2}+g_{22}(dy^{2})^{2}\, $

In general the metric tensor $ \mathbf {g} \, $ is a function of position. The terms $ g_{11}\, $ and $ g_{22}\, $ describe the relative spread of the axes, while $ g_{12}\, $ describes how the axes are not perpendicular.

A particular geometry is called Flat if it can be described by a Euclidian geometry. In general, curved manifolds (such as the surface of a sphere) require a more complex metric.

Example: Metric Tensor in Polar Coordinates

Consider polar coordinates in Euclidean space:

$ x=r\cos(\theta ),\;y=r\sin(\theta ) $

The differential distance is given by:

$ \mathrm {d} s^{2}=\mathrm {d} x^{2}+\mathrm {d} y^{2}=\mathrm {d} r^{2}+r^{2}\mathrm {d} \theta ^{2}\, $

which shows the components of the metric tensor are:

$ g_{rr}=1,\;g_{\theta \theta }=r^{2},\;g_{r\theta }=0 $

Transformation

Now consider a general transformation between two general CS $ x, $ and $ y, $, and a scalar field $ \phi , $. The scalar field does not depend on the CS used, thus:

$ \phi (y)=\phi (x); $.

Now,

Contravariant vector transformation:

$ V^{n}(y)={\frac {\partial y^{n}}{\partial x^{m}}}V^{m}(x) $

Covariant vector transformation:

$ V_{n}(y)={\frac {\partial x^{m}}{\partial y^{n}}}V_{m}(x) $

Derivative of a Tensor

Scalar

Consider a scalar field $ \phi \, $. Clearly the value of the field at any point P is independent of the CS used to label P. If the field is constant on one CS, will be constant in any CS. Note that:

$ {\frac {\partial \phi }{\partial x^{m}}} $

is a vector.

Vector

Now consider a constant vector field $ \mathbf {V} $ in flat space, in the Cartesian CS. The covariant components of $ \mathbf {V} $ are also constant - that is, the projections on the axes:

$ {\frac {\partial V_{m}}{\partial x^{n}}}=0 $.

If the vector field is now labelled by a general curvilinear CS, we see that the components of the vectors now change over position, even if the vector is constant, because the CS is not "constant":

$ {\frac {\partial V_{m}}{\partial x^{n}}}=0 $.

Moreover:

$ {\frac {\partial V_{m}(x)}{\partial x^{n}}}=0\Rightarrow {\frac {\partial V_{m}(y)}{\partial y^{n}}}=0 $

which states that vectors do not transform as tensors under a CS change.

Covariant Derivative

We would like to find a new definition of a derivative that maps a vector to a vector, and a tensor to a tensor. "Covariant" in this context means the quantity is independent of the CS chosen. Suppose there exists:

$ T_{mn}(x)={\frac {\partial V_{m}}{\partial x^{n}(x)}} $

So:

$ T_{mn}(y)={\frac {\partial x^{r}}{\partial y^{m}}}{\frac {\partial x^{s}}{\partial y^{n}}}T_{sr}(x)={\frac {\partial x^{r}}{\partial y^{m}}}{\frac {\partial x^{s}}{\partial y^{n}}}{\frac {\partial V_{r}(x)}{\partial x^{s}}} $

Now compare with (expanding):

$ {\frac {\partial V_{m}(y)}{\partial y^{n}}}={\frac {\partial }{\partial y^{n}}}{\frac {\partial x^{r}}{\partial y^{m}}}V_{r}(x)={\frac {\partial x^{r}}{\partial y^{m}}}{\frac {\partial V_{r}(x)}{\partial y^{n}}}+{\frac {\partial }{\partial y^{n}}}{\frac {\partial x^{r}}{\partial y^{m}}}V_{r}(x) $

The first term is equal to $ T_{mn}(y)\, $, but we have a second term, which we denote by $ \Gamma ^{r}{}_{mn}\, $

Hence in gernal we need to differentiate in a way to cancel the second term to get back a tensor:

$ \nabla _{p}T_{mn}={\frac {\partial T_{mn}}{\partial y^{p}}}+\Gamma ^{r}{}_{pm}T_{rn}+\Gamma ^{r}{}_{pm}T_{mr} $

The Christoffel Symbols can be found from the metric tensor:

$ \Gamma ^{a}{}_{bc}(y)={\frac {1}{2}}g^{ad}\left({\frac {\partial g_{dc}}{\partial y^{b}}}+{\frac {\partial g_{db}}{\partial y^{c}}}-{\frac {\partial g_{bc}}{\partial y^{d}}}\right) $

Parallel Transport and Curvature

Space is called "flat" (like Cartesian space) when it is possible to choose a CS such that the covariant derivavtive of the metric tensor is everywhere zero:

$ \nabla _{r}g^{mn}=0 $ that is the metric tensor reduces to the delta function: $ g_{mn}=\delta _{mn}\, $

A space may be flat in some areas, but there may be curvature at other points. It is always possible to choose a CS such that at a given point, the derivavtive of the metric is zero - that is in, a small enough neighbourhood of any point of a continuous, differentiable space looks flat.

Consider a vector V moving from point A to B over a curve, whilst remaining parallel to itself. This is notion of parallel transport, and can be extended to general nonflat spaces. The covariant derivavtive:

$ \nabla _{s}V^{m}={\frac {dV^{m}}{ds}}+\Gamma ^{m}{}_{np}V^{n}{\frac {dx^{p}}{ds}} $

If a vector is parallel transported such that the covariant derivative is always zero, the vector follows a geodesic; geodesics are in some sense the "straightest" lines that exist in the manifold. For example: all straight lines in flat 2D space are geodesics; on the surface of a sphere, all great circles are geodesics.

The geodesic condition is:

$ {\frac {d^{2}x^{m}}{ds^{2}}}+\Gamma ^{m}{}_{np}{\frac {dx^{n}}{ds}}{\frac {dx^{p}}{ds}}=0 $