6.4 Radial Paths in a Spherically Symmetrical Field 

It is no longer clear which way is up even if one wants to rise. 
David Riesman, 1950 

In this section we consider the simple spacetime trajectory of a test particle moving radially with respect to a spherical mass. By “test particle” we mean a particle that is sufficiently small in comparison with the gravitating spherical mass so that the particle’s contribution to the overall gravitational field is negligible. Hence we are really just evaluating empty geodesic trajectories in the spacetime surrounding the central mass, i.e., we are considering the onebody problem. As we saw in Section 6.1, the field equations of general relativity imply that the metric of spacetime in the region surrounding an isolated spherical mass m can be written as 
where t is the time coordinate, r is the radial coordinate, q and f are the usual angles for polar coordinates, and τ is the proper time. Since we're interested in purely radial motions, the differentials of the angles dq and df are zero, and we're left with a twodimensional surface with the coordinates t and r, with the metric 

Thus the metric tensor for this twodimensional space is given by the diagonal matrix 

which has determinant g = 1. The inverse of the covariant tensor g_{uv} is the contravariant tensor 

To make use of index notation we define x^{1} = t and x^{2} = r, and then the equations for the geodesic paths in this manifold can be expressed as 

where summation is implied over any indices that are repeated in a given product, and G^{i}_{jk} denotes the Christoffel symbols. Note that the index i can be either 1 or 2, so the above expression actually represents two differential equations involving the 1st and 2nd derivatives of our coordinates x^{1} and x^{2} (which, remember, are just t and r) with respect to the proper time t for timelike paths. 
The Christoffel symbol is defined in terms of the partial derivatives of the components of the metric tensor as follows 

Taking the partials of the components of our g_{uv} with respect to t and r we find that they are all zero, with the exception of 

Combining this with the fact that the only nonzero components of the inverse metric tensor g^{uv} are g^{11} and g^{22}, we find that the only nonzero Christoffel symbols are 



So, substituting these expressions into the geodesic formula (2), and reverting back to the symbols t and r for our coordinates, we have the two ordinary differential equations for the geodesic paths on the surface 

These equations can be integrated in closed form (see below), but they can also be directly integrated numerically using small incremental steps of dτ. For any given initial position and trajectory we can generate the subsequent geodesic path in terms of r as a function of t. We find that such paths invariably go to infinite t as r approaches 2m. Is our twodimensional surface actually singular at r = 2m, or are the coordinates simply illbehaved (like longitude at the North pole)? 
As we saw above, the surface has an invariant Gaussian curvature at each point. Let's determine the curvature to see if anything strange occurs at r = 2m. The curvature can be computed in terms of the components of the metric tensor and their first and second partial derivatives. The nonzero first derivatives for our surface (and the determinant g = 1) were noted above. The only nonzero second derivatives are 

So we can compute the intrinsic curvature of our surface using Gauss's formula for the curvature invariant K of a twodimensional surface given in Section 5.3. Inserting the metric components and derivatives for our surface into that equation gives the intrinsic curvature 

Therefore, at r = 2m the curvature of this surface is 1/(4m^{2}), which is certainly finite, and in fact can be made arbitrarily small for sufficiently large m. The only singularity in the intrinsic curvature of the surface occurs at r = 0. 
In order to solve the geodesic equations (3) for r as a function of the proper time t we first rewrite the second geodesic equation in the form 

Since the basic line element (1) implies 

it follows that the quantity in the square brackets in (4) is unity, so we have 

Furthermore, notice that the derivative with respect to τ of the expression on the right hand side equation (5) is 

where we’ve made use of equation (6). Therefore, the expression in the square brackets on the left side is a constant (corresponding to the constant sum of potential plus kinetic energy), whose value for any given trajectory can be determined at any convenient point. For a bounded trajectory there is a radial position R, the apogee of the path, where dr/dτ = 0, and hence for any such trajectory we have 

On the other hand, for an unbounded trajectory there is no apogee, but instead the velocity dr/dt approaches an asymptotic value V as r goes to infinity. Noting that dr/dτ = (dr/dt)(dt/dτ) and making use of the basic line element (1) to give dt/dτ in terms of dr/dt, we have 

Therefore, for an unbounded radial trajectory with asymptotic speed V we have 

As an aside, we note that although we’ve asserted that the quantity in square brackets on the right side of equation (4) is unity, the denominator is zero at r = 2m, so the expression is actually singular at that point. However, it is a removable singularity, because the numerator also goes to zero at r = 2m, canceling the zero in the denominator. This implies that (dr/dt)^{2} is invariably forced to 1  2m/R precisely at r = 2m for bounded trajectories, and to 1/(1−V^{2}) for unbounded trajectories. 
Focusing on bounded trajectories, we return to (7a) and note that it implies 

Taking the square root and rearranging terms, this gives 

We have the integral 

To simplify this result, we make a change of variables by defining the argument of the inverse sine to be the cosine of some angle a. Thus we define a such that cos(a) = 2r/R – 1, which implies 

Inserting this into the preceding equation gives the elapsed proper time between r_{1} = R and r_{2} = r as 

This shows that equation (6) has the same closedform solution as does radial freefall in Newtonian mechanics (as shown in Section 4.3 if t is identified with Newton's coordinate time t), namely, the parametric "cycloid relations". A plot of this r versus t corresponds to the position of a point on the rim of a rolling wheel of radius R/2, where a is the angle of the wheel. 
We can also express the Schwarzschild coordinate time t explicitly in terms of a by multiplying the two relations 

to give 

Substituting the parametric expression for r into this equation, multiplying through by da, and integrating both sides, we get 

The integral can be evaluated explicitly to give 

Now, making use of the trigonometric identity 

the equation can be written in the form 

where Q = . For values of a corresponding to r < 2m the argument of the logarithm is negative, and hence the value of the logarithm is offset by pi. This occurs because, in such cases, we are integrating from a = 0 where r = R (which is greater than 2m) to a value of a corresponding to r less than 2m, and hence we must perform a complex integration around the singularity at r = 2m, offsetting the result by ±pi (assuming the path of integration doesn’t make any complete loops around the singularity). This is not surprising, because the t coordinates are discontinuous at r = 2m, so we cannot unambiguously “carry over” the labeling of the t coordinates in the region r > 2m to the region r < 2m. In general, since the metric coefficients are independent of t, the t labels for events outside r = 2m can all be offset by a constant value without affecting any of our results, and likewise the t labels for events inside r = 2m can all be offset by a constant value. Moreover, the t label offsets for the inner and outer regions are independent of each other, because of the discontinuity at r = 2m. Lacking any definite interior boundary condition, we are free to choose the interior offset such that t is realvalued. The real part of ln(z) for any complex z, positive or negative, is ln(z), so we can simply stipulate that we will take the absolute value of the argument of the logarithm, i.e., we define the t coordinates by 

This gives a purely realvalued labeling of the t coordinates that satisfies the condition on the derivative at every point (except of course where the t coordinates are singular at r = 2m). Strictly speaking, we could further offset the interior labels by any real constant, so the above expression for the coordinate time of a freefalling particle is not unique, but it is the simplest matching of the t labels. On this basis, a typical timelike radial orbit is illustrated below, both in terms of proper time and Schwarzschild coordinate time, as function of the parameter a. 

A notable feature of this trajectory is its temporal symmetry. Not only is there a continuous geodesic path from the apogee down through the Schwarzschild radius to the singularity at r = 0, there is also a continuous geodesic path from the singularity up through the Schwarzschild radius to the apogee. This was to be expected in view of the temporal symmetry of the field equations in general, and the Schwarzschild metric in particular, but it might seem inconsistent with the wellknown fact that once a particle has crossed from outside to inside the Schwarzschild radius it can never reemerge. However, there is no inconsistency, because the emerging particle has never crossed from outside to inside that radius. 
To understand the full set of possible trajectories consistent with the Schwarzschild metric, it’s useful to first note an ambiguity present in all pseudoRiemannian metrics due to their quadratic character. Consider the Minkowski metric (dt)^{2} = (dt)^{2} – (dx)^{2}, which obviously doesn’t constrain the signs of the differentials, because they each appear squared. At constant x this metric requires (dt/dt)^{2} = 1, but the ratio dt/dt itself can be either +1 or −1. Strictly speaking, we are free to choose whether the proper time along a given path increases or decreases as the coordinate time increases. We might fancifully imagine that the Minkowski metric actually entails two separate universes, with proper time increasing with coordinate time in one, and decreasing with coordinate in the other. Alternatively we could imagine a single universe with two families of particles, whose proper times increase in opposite directions of the coordinate time t. (In fact, John Wheeler once speculated that antimatter particles might be modeled as particles moving backward in time.) However, with a fixed metric like the Minkowski metric, it’s easy to just arbitrarily stipulate the same sign for dt and dt for every path, and then continuity requires that this always remains true (since timelike paths cannot “turn around” in Minkowski space). 
The same quadratic ambiguity arises when considering the Schwarzschild metric, but in this case the various possible signs of the differentials are more interrelated, because the coefficients of the metric change signs at r = 2m. For values of r greater than 2m we have a metric of the form (dt)^{2} = (dt)^{2} – (dr)^{2} neglecting scale factors, whereas for values of r less than 2m the metric takes the form (dt)^{2} = (dr)^{2} – (dt)^{2}. In the former case, dt must always equal or exceed dt, but in the latter case dr must equal or exceed dt. Thus, outside the Schwarzschild radius we must choose the sign of dt/dt, and inside that radius we must choose the sign of dr/dt. The signs of these ratios cannot change along any particle’s path in their respective regions. In effect, the radius r serves as the “time” coordinate inside the Schwarzschild radius. 
Now, by analytic continuation, it can be shown that a path crossing the Schwarzschild radius from an outer region must enter an inner region with negative dr/dt. This is why a particle falling inward through the Schwarzschild radius must thereafter continue to reach smaller and smaller values of r. It cannot “turn around”, but must continue down to r = 0. However, conversely, it can be shown that a particle passing outward through the Schwarzschild radius must have come from an inner region of positive dr/dt. Hence if we observe objects falling into the inner region, and other objects emerging from the inner region, we seem forced to conclude that there are two physically distinct inner regions, or else that there exist closed spacetime loops if we insist on a single interior region. One or the other of these consequences is unavoidable if we take seriously the analytic continuation of all geodesics consistent with the Schwarzschild metric. The existence of two distinct inner regions is perhaps not surprising if we note that an infalling object requires infinite coordinate time to cross the boundary at r = 2m, and conversely an outgoing object requires infinite coordinate time to emerge. Clearly these are two very different classes of objects, one coming from the beginning of coordinate time, and the other departing to the end of coordinate time. The same reasoning leads to the potential existence of a second outer region, with negative dt/dt, so the full extent of the manifold entailed by the Schwarzschild metric, if fully developed, consists of four distinct regions. Thus the consideration of simple radial trajectories in Schwarzschild spacetime leads unavoidably to cosmological issues, which are described more fully in the discussions of “black holes” in Section 7. 
In the preceding discussion we have focused on timelike radial paths, taking the proper time τ as the path length parameter. As noted in Section 6.1, for lightlike paths we have dτ = 0 and so the metric (1) reduces to simply (1 – 2m/r)^{2}(dt)^{2} = (dr)^{2}, and thus we have, for any r_{2} and r_{1} greater than 2m, the coordinate time difference 

As expected, if m = 0 this reduces to (t_{2} – t_{1}) = ±(r_{2} – r_{1}). For nonzero m, we see that dr/dt = 0 at r = 2m (where these coordinates are illconditioned), and it isn’t obvious from this expression how to extrapolate through that boundary. 
One way of clarifying all possible radial paths, timelike and lightlike, consistent with the Schwarzschild solution is to rewrite the radial line element (1) as 

If we define a new radial coordinate r so that the second term in the square brackets is (dr)^{2}, then light rays will be diagonal lines when plotted in terms of t and r. Thus we set 

Notice that either sign is possible, since only the squared differential appears in (9). Integrating both sides and choosing a suitable constant of integration, we define r explicitly by 

The absolute value is used to reverse the signs at r = 2m, so that the argument of the logarithm is always nonnegative. (Note that the derivative of r with respect to r is invariant under reversal of sign of the argument of the logarithm.) This relation can also be written in the form 

so we can write the radial Schwarzschild line element (9) in the form 

where r is now regarded as a function of r. The leading coefficient on the right side is wellbehaved except at r = 0, but the trailing coefficient is singular at r = 2m, where r is infinite. Since dt is finite at that point, we infer that (dt)^{2} – (dr)^{2} must be identically zero at that point. We wish to absorb the trailing coefficient into the differentials to give an explicitly finite expression for (dt)^{2}. Notice that in terms of coordinates A and B defined such that r = A+B and t = AB the line element has the form 

Recalling that d(e^{x}) = e^{x}dx, we see that we can absorb the exponential coefficients into the differentials by simply defining the coordinates 

The line element in terms of these coordinates has the simple form 

For convenience we can now return to the orthogonal hyperbolic form by making one more change of coordinates, defining u and v such that U = u+v and V = uv. Making these substitutions, we get 

where, as noted previously, the parameter r is treated as a function of u and v. These are called KruskalSzekeres coordinates. Making all the substitutions for the changes of variables, we see that they are given explicitly as functions of r and t by 

The signs for the case r < 2m are positive in the collapsing interior region and negative in the expanding interior region. A plot of the Schwarzschild solution in terms of these coordinates is shown below. 

The dotted curve represents a complete timelike radial geodesic. As discussed previously, this curve is temporally symmetrical, emerging from the r = 0 singularity, rising through the r = 2m horizon to the apogee (which is at 2.5m in this plot), and then falling back through the r = 2m horizon to the singularity at r = 0. These coordinates confirm that there are actually two singularities in this fully developed solution. The lower r = 0 locus in the plot is the singularity at the center of a “white hole”, and r is always increasing with proper time in the region surrounding this singularity. The upper r = 0 locus is the singularity at the center of a “black hole”, and r is always decreasing with proper time in the region surrounding this singularity. The spatial region to the right of the v axis is our usual external universe, whereas the mirror region on the left is a separate universe. However, the physical applicability of this analytically complete solution is highly dubious, because no known physical process would lead to such a result. The “black holes” to be discussed in Section 7, hypothesized to result from the gravitational collapse of stars, do not entail this complete solution, so the global topology of the complete Schwarzschild solution, as exhibited by the Kruskal coordinates, is presumably of only theoretical interest. 
