Zero divergence of energy-momentum tensor and gravitational energy

Question

Trying to teach myself general relativity and have just hit yet another confusion. I'm reading that in curved spacetime the energy-momentum tensor has zero divergence, ie

$$\nabla_{\mu}T^{\mu\nu}=0.$$

But that this doesn't imply the total conservation of energy and momentum as there is an additional source of energy (the gravitational field) that isn't included in the EMT. If that's the case, and if the EMT doesn't describe the total energy of system, how is it valid to use the tensor to describe various systems. For example, $$T^{\mu\nu}=0$$ for the Schwarzschild solution, or assuming spacetime is a perfect fluid in cosmology? How are these assumptions valid if they don't include the energy contribution of the gravitational field? Seems a bit of an elephant in the room-type situation. Or is that energy so small it can be ignored?

Thank you

This post imported from StackExchange Physics at 2014-03-22 17:20 (UCT), posted by SE-user Peter4075

Answer 1

The actual reason why one can't interpret the equation $$ \nabla_\mu T^{\mu\nu}=0 $$ as a global conservation law is that it uses covariant derivatives. If a law like that were valid with partial derivatives, you could derive such a law. But there's a covariant derivative which is one of the technical ways to explain that general relativity in generic backgrounds doesn't preserve any energy:

http://motls.blogspot.com/2010/08/why-and-how-energy-is-not-conserved-in.html

The text above also explains other reasons why the conservation law disappears in cosmology.

However, despite the non-existence of a global (nonzero) conserved energy in general backgrounds, the tensor $T_{\mu\nu}$ is still well-defined. As twistor correctly writes, it quantifies the contribution to the energy and momentum from all matter fields (non-gravitational ones) and matter particles. And if you can approximate the background spacetime by a flat one, $g_{\mu\nu}=\eta_{\mu\nu}$, which is usually the case with a huge precision (in weak enough gravitational fields, locally, or if you replace local objects that heavily curve the spacetime, including black holes, by some effective $T$, using a very-long-distance effective description), then $\nabla$ may be replaced by $\partial$ in the flat Minkowski coordinates and the situation is reduced to that of special relativity and the "integral conservation law" may be restored.

This post imported from StackExchange Physics at 2014-03-22 17:20 (UCT), posted by SE-user Luboš Motl

Comments

Again, the divergence of $T$ is zero but it is the covariant divergence. The covariant derivative contains extra terms of the form $\Gamma T$ with some indices contracted which are not derivatives. If you integrate these terms over a spatial slice, you won't be able to use the Gauss' law because there are no derivatives in this term, so you won't be able to convert these terms to fluxes through the surface. Because of the difference between the partial and covariant derivative, there's no integral version of the law. Haven't I written it? Do you need this to be written more slowly?

This post imported from StackExchange Physics at 2014-03-22 17:20 (UCT), posted by SE-user Luboš Motl

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thanks. Any chance of more slowly and even simplier, with no reference to Lagrangians? I have a rudimentary understanding of the divergence theorem, connection coefficients and covariant derivatives. My understanding of divergence is at the level of sources and sinks of a liquid sloshing about in a container - if no liquid is entering or leaving the container, the divergence equals zero. I'm trying to relate that simple picture to $\nabla_{\mu}T^{\mu\nu}=0$ and why that implies the conservation of energy in flat but not in curved spacetime.

This post imported from StackExchange Physics at 2014-03-22 17:20 (UCT), posted by SE-user Peter4075

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Is it possible to describe, in absolute baby steps why that implication is true?

This post imported from StackExchange Physics at 2014-03-22 17:20 (UCT), posted by SE-user Peter4075

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The only sentence in which I mentioned Lagrangians was when I said that you may calculate the formula for the stress-energy tensor out of the Lagrangian. If you can't use the Lagrangians, you won't be able to derive the stress-energy tensor in this way and you may ignore this sentence. You will have to use an explicit God-given formula for $T$. But otherwise nothing whatsoever changes about the remaining things I said. For the equivalence of global and local continuity equation - conservation laws - see en.wikipedia.org/wiki/Continuity_equation . It uses $\partial$, not $\nabla$.

This post imported from StackExchange Physics at 2014-03-22 17:20 (UCT), posted by SE-user Luboš Motl

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apologies for being a bit slow on the uptake. This stuff would be a lot easier if (a) I was smarter and (b) I had a degree in physics. I confess I've only just today found out what a continuity equation is! I've also just read a reasonably understandable on-line piece by Weiss and Baez titled, "Is energy conserved in general relativity". Their answer is an unambiguous, "In special cases, yes. In general — it depends on what you mean by 'energy', and what you mean by 'conserved'." Glad that's sorted out.

This post imported from StackExchange Physics at 2014-03-22 17:20 (UCT), posted by SE-user Peter4075

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in some way from the rhs, hence my confusion. I didn't know that (as you say) “the curvature of spacetime is ONLY dictated by the density of the non-gravitational energy density T or EMT”. So, thankfully, all the calculations I've struggled through re Schwarzschild and cosmology are still valid because only the EMT (and not gravitational energy) curves spacetime? I'm still puzzled about why zero divergence of the rhs (the EMT) doesn't imply the conservation of energy and momentum. If you put the Einstein tensor on the rhs (ie, the lhs equals zero), would the zero divergence

This post imported from StackExchange Physics at 2014-03-22 17:20 (UCT), posted by SE-user Peter4075

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of the rhs (the EMT) doesn't imply the conservation of energy and momentum. If you put the Einstein tensor on the rhs (ie, the lhs equals zero), would the zero divergence of the rhs then imply total conservation of energy and momentum?

This post imported from StackExchange Physics at 2014-03-22 17:20 (UCT), posted by SE-user Peter4075

Answer 2

The stress-energy tensor describes the energy momentum content contributed by all the fields present with the exception of the gravitational field itself. However, just because it doesn't appear in the energy momentum tensor does not mean that gravity can't act, in some sense, as a source of gravity. The Einstein equations are nonlinear, and from this nonlinearity arises the possibility for gravity to "gravitate" in a consistent way.

Attempts to describe the energy-momentum of the gravitational field itself locally (as you would need to do if you wished to include a gravitational field contribution in the stress energy tensor) are known to run into problems. By locally I mean that we would try to write down a tensor field that encapsulates the gravitational field energy-momentum at each point.

This post imported from StackExchange Physics at 2014-03-22 17:20 (UCT), posted by SE-user twistor59