Schwarzschild coordinates


In the theory of Lorentzian manifolds, spherically symmetric spacetimes admit a family of nested round spheres. In such a spacetime, a particularly important kind of coordinate chart is the Schwarzschild chart, a kind of polar spherical coordinate chart on a static and spherically symmetric spacetime, which is adapted to these nested round spheres. The defining characteristic of Schwarzschild chart is that the radial coordinate possesses a natural geometric interpretation in terms of the surface area and Gaussian curvature of each sphere. However, radial distances and angles are not accurately represented.
These charts have many applications in metric theories of gravitation such as general relativity. They are most often used in static spherically symmetric spacetimes. In the case of general relativity, Birkhoff's theorem states that every isolated spherically symmetric vacuum or electrovacuum solution of the Einstein field equation is static, but this is certainly not true for perfect fluids. We should also note that the extension of the exterior region of the Schwarzschild vacuum solution inside the event horizon of a spherically symmetric black hole is not static inside the horizon, and the family of nested spheres cannot be extended inside the horizon, so the Schwarzschild chart for this solution necessarily breaks down at the horizon.

Definition

Specifying a metric tensor is part of the definition of any Lorentzian manifold. The simplest way to define this tensor is to define it in compatible local coordinate charts and verify that the same tensor is defined on the overlaps of the domains of the charts. In this article, we will only attempt to define the metric tensor in the domain of a single chart.
In a Schwarzschild chart, the line element takes the form
Where is the standard spherical coordinate and is the standard metric on the unit 2-sphere. See Deriving the Schwarzschild solution for a more detailed derivation of this expression.
Depending on context, it may be appropriate to regard a and b as undetermined functions of the radial coordinate. Alternatively, we can plug in specific functions to obtain a Schwarzschild coordinate chart on a specific Lorentzian spacetime.
If this turns out to admit a stress–energy tensor such that the resulting model satisfies the Einstein field equation, then, with appropriate tensor fields representing physical quantities such as matter and momentum densities, we have a piece of a possibly larger spacetime; a piece which can be considered a local solution of the Einstein field equation.

Killing vector fields

With respect to the Schwarzschild chart, the Lie algebra of Killing vector fields is generated by the timelike irrotational Killing vector field
and three spacelike Killing vector fields
Here, saying that is irrotational means that the vorticity tensor of the corresponding timelike congruence vanishes; thus, this Killing vector field is hypersurface orthogonal. The fact that our spacetime admits an irrotational timelike Killing vector field is in fact the defining characteristic of a static spacetime. One immediate consequence is that the constant time coordinate surfaces form a family of spatial hyperslices.

A family of static nested spheres

In the Schwarzschild chart, the surfaces appear as round spheres, and from its form, we see that the Schwarzschild metric restricted to any of these surfaces is positive definite and given by
Where is the standard Riemannian metric on the unit radius 2-sphere. That is, these nested coordinate spheres do in fact represent geometric spheres with
  1. surface area
  2. Gaussian curvature
In particular, they are geometric round spheres. Moreover, the angular coordinates are exactly the usual polar spherical angular coordinates: is sometimes called the colatitude and is usually called the longitude. This is essentially the defining geometric feature of the Schwarzschild chart.
It may help to add that the four Killing fields given above, considered as abstract vector fields on our Lorentzian manifold, give the truest expression of both the symmetries of a static spherically symmetric spacetime, while the particular trigonometric form which they take in our chart is the truest expression of the meaning of the term Schwarzschild chart. In particular, the three spatial Killing vector fields have exactly the same form as the three nontranslational Killing vector fields in a spherically symmetric chart on E3; that is, they exhibit the notion of arbitrary Euclidean rotation about the origin or spherical symmetry.
However, note well: in general, the Schwarzschild radial coordinate does not accurately represent radial distances, i.e. distances taken along the spacelike geodesic congruence which arise as the integral curves of. Rather, to find a suitable notion of 'spatial distance' between two of our nested spheres, we should integrate along some coordinate ray from the origin:
Similarly, we can regard each sphere as the locus of a spherical cloud of idealized observers, who must use rocket engines to accelerate radially outward in order to maintain their position. These are static observers, and they have world lines of form, which of course have the form of vertical coordinate lines in the Schwarzschild chart.
In order to compute the proper time interval between two events on the world line of one of these observers, we must integrate along the appropriate coordinate line:

Coordinate singularities

Looking back at the coordinate ranges above, note that the coordinate singularity at
marks the location of the North pole of one of our static nested spheres, while marks the location of the South pole. Just as for an ordinary polar spherical chart on E3, for topological reasons we cannot obtain continuous coordinates on the entire sphere; we must choose some longitude to act as the prime meridian and cut this out of the chart. The result is that we cut out a closed half plane from each spatial hyperslice including the axis and a half plane extending from that axis.
When we said above that is a Killing vector field, we omitted the pedantic but important qualifier that we are thinking of as a cyclic coordinate, and indeed thinking of our three spacelike Killing vectors as acting on round spheres.
Possibly, of course, or, in which case we must also excise the region outside some ball, or inside some ball, from the domain of our chart. This happens whenever f or g blow up at some value of the Schwarzschild radial coordinate r.

Visualizing the static hyperslices

To better understand the significance of the Schwarzschild radial coordinate, it may help to embed one of the spatial hyperslices in a flat Euclidean space. People who find it difficult to visualize four-dimensional Euclidean space will be glad to observe that we can take advantage of the spherical symmetry to suppress one coordinate. This may be conveniently achieved by setting. Now we have a two-dimensional Riemannian manifold with a local radial coordinate chart,
To embed this surface in E3, we adopt a frame field in E3 which
  1. is defined on a parameterized surface, which will inherit the desired metric from the embedding space,
  2. is adapted to our radial chart,
  3. features an undetermined function.
To wit, consider the parameterized surface
The coordinate vector fields on this surface are
The induced metric inherited when we restrict the Euclidean metric on E3 to our parameterized surface is
To identify this with the metric of our hyperslice, we should evidently choose such that
To take a somewhat silly example, we might have.
This works for surfaces in which true distances between two radially separated points are larger than the difference between their radial coordinates. If the true distances are smaller, we should embed our Riemannian manifold as a spacelike surface in E1,2 instead. For example, we might have. Sometimes we might need two or more local embeddings of annular rings. In general, we should not expect to obtain a global embedding in any one flat space.
The point is that the defining characteristic of a Schwarzschild chart in terms of the geometric interpretation of the radial coordinate is just what we need to carry out this kind of spherically symmetric embedding of the spatial hyperslices.

A metric Ansatz

The line element given above, with f,g regarded as undetermined functions of the Schwarzschild radial coordinate r, is often used as a metric ansatz in deriving static spherically symmetric solutions in general relativity.
As an illustration, we will indicate how to compute the connection and curvature using Cartan's exterior calculus method. First, we read off the line element a coframe field,
where we regard are as yet undetermined smooth functions of. .
Second, we compute the exterior derivatives of these cobasis one-forms:
Comparing with Cartan's first structural equation,
we guess expressions for the connection one-forms.
If we recall which pairs of indices are symmetric and which are antisymmetric in, we can confirm that the six connection one-forms are
We can collect these one-forms into a matrix of one-forms, or even better an SO-valued one-form.
Note that the resulting matrix of one-forms will not quite be antisymmetric as for an SO-valued one-form; we need to use instead a notion of transpose arising from the Lorentzian adjoint.
Third, we compute the exterior derivatives of the connection one-forms and use Cartan's second structural equation
to compute the curvature two forms. Fourth, using the formula
where the Bach bars indicate that we should sum only over the six increasing pairs of indices, we can read off the linearly independent components of the Riemann tensor with respect to our coframe and its dual frame field. We obtain:
Fifth, we can lower indices and organize the components into a matrix
where E,L are symmetric and B is traceless, which we think of as representing a linear operator on the six-dimensional vector space of two forms. From this we can read off the Bel decomposition with respect to the timelike unit vector field. The electrogravitic tensor is
The magnetogravitic tensor vanishes identically, and the topogravitic tensor, from which we can determine the three-dimensional Riemann tensor of the spatial hyperslices, is
This is all valid for any Lorentzian manifold, but we note that in general relativity, the electrogravitic tensor controls tidal stresses on small objects, as measured by the observers corresponding to our frame, and the magnetogravitic tensor controls any spin-spin forces on spinning objects, as measured by the observers corresponding to our frame.
The dual frame field of our coframe field is
The fact that the factor only multiplies the first of the three orthonormal spacelike vector fields here means that Schwarzschild charts are not spatially isotropic ; rather, the light cones appear or. This is of course just another way of saying that Schwarzschild charts correctly represent distances within each nested round sphere, but the radial coordinate does not faithfully represent radial proper distance.

Some exact solutions admitting Schwarzschild charts

Some examples of exact solutions which can be obtained in this way include:
It is natural to consider nonstatic but spherically symmetric spacetimes, with a generalized Schwarzschild chart in which the metric takes the form
Generalizing in another direction, we can use other coordinate systems on our round two-spheres, to obtain for example a stereographic Schwarzschild chart which is sometimes useful: