Reference: Moore, Thomas A., *A General Relativity Workbook*, University Science Books (2013) – Chapter 17; Box 17.1.

It’s time to return to the study of tensors so we can pave the way for the Einstein equation which is the basis of general relativity. Up to now, we’ve assumed that the Schwarzschild metric described spacetime outside a spherical mass, without any arguments to back up this assumption. Developing these arguments requires some more tools from the tensor toolbox.

One problem with tensors is that their straightforward derivatives are not, in general, tensors themselves. For example, the first derivative of a scalar function is a covariant tensor, as it transforms according to

If we take the derivative of this equation with respect to another of the primed coordinates , we get

where we used the chain rule on the second term. In order for to transform like a tensor, the first term in the last line would have to be zero, but it’s clearly not, in general.

To remedy this problem, first cast your mind back to the definition of basis vectors in some coordinate system. The basis vectors are linearly independent vectors that are tangent to the lines of constant coordinate values and that span the space. They must satisfy

where is the metric tensor. Keep in mind that, for a general coordinate system, these basis vectors need not be either orthogonal or unit vectors, and that they can change as we move around. As such, we can consider the derivative of basis vector with respect to coordinate with all other coordinates held constant. Since the derivative of a vector is another vector, and the basis vectors span the space, we can express this derivative as a linear combination of the basis vectors at the point at which the derivative is taken. That is

The quantities are called **Christoffel symbols**, named after Elwin Bruno Christoffel, a 19th century German mathematician and physicist. (Students of GR often refer to them as the ‘Christ-awful’ symbols, since formulas involving them can be tricky to use and remember due to the number of indices involved.) It’s important to note that although is written with indices that make it look like a tensor, it is **not** a tensor on its own. The transformation equation for can be derived from its explicit form (which we haven’t got to yet), but for reference here it is:

The first term is the normal transformation for a rank-3 tensor, but the second term spoils the transformation. However, notice that if we use the special coordinate transformation where and , then the second derivative in the second term vanishes, since and are independent variables in the same coordinate system, so none of them depends on the others. Furthermore, in this special case , so the transformation becomes

which is a valid tensor transformation. That is, the Christoffel symbol’s upper index does transform as a tensor, which makes sense, since 8 defines a four-vector with components , holding and fixed.

We’ll get to methods for calculating Christoffel symbols in a later post. For now, we’ll see how we can define a derivative of a tensor that is itself always another tensor. Suppose we have a vector field . In a given coordinate system, we can write this in terms of the basis vectors:

If we calculate its differential we get

where in line 16 we relabelled the index to in the first term, and in line 17 we defined the **absolute gradient**:

The combination has only one free index , and it appears in the form

so that is component of a four-vector. Since the differential is a tensor, the absolute gradient must also be a tensor of rank 2. We’ve thus found a derivative of a tensor (well, just a four-vector so far) that is itself a tensor. The term ‘absolute gradient’ seems to be peculiar to Moore’s book; it’s more commonly known as the **covariant derivative**.

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