# What is the physical intepretation of harmonic coordinates?

When I see harmonic coordinates used somewhere, what should my association be?

Is there some general use or need to consider the harmonic cooridnate condition?

I don't really see what's behind all the things said in the wikipedia article and I've seen these coordinates used in some papers but don't really understan their significance, other than that one can consequently algebraically use the relation $\Delta x^\mu=0$ in computations. I don't see what that means though, do the full set of these coordinates have some general geometrically visible properties, maybe characterized with the associated base of distributions?

Moreover, do these cooridnates have some special role in geometric quantization?

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Since when have people started calling this "Harmonic Coordinates" ? I learnt it as the de Donder Gauge, but I see that wikipedia lists it as harmonic coordinates. Though, they also list a certain famous theory of spontaneous symmetry breaking with only one name attached, so maybe I should pay it less heed. –  Flint72 May 24 at 10:39

The well known property of the harmonic coordinates is that the covariant divergence of a vector field and the d'Alambertian of a scalar field take a particularly simple form: $$D_{\mu}A^{\mu} \rightarrow g^{\mu\nu}\partial_{\mu}A_{\nu},\\ g^{\mu\nu}D_{\nu}D_{\mu}\phi \rightarrow g^{\mu\nu}\partial_{\mu} \partial_{\nu}\phi.$$ The harmonic condition $$\partial_{\mu}\left( \sqrt{-g}g^{\mu\nu}\right) =0\qquad\qquad\left( 1\right)$$ is widely used to construct the so called de Donder gauge for the quantization of a weak gravitational field. If one uses the deviation $\psi^{\mu\nu}$ of the contravariant metric density from the flat one $\eta^{\mu\nu}=diag\left( 1,-1,-1,-1\right)$ as a field variable: $$\sqrt{-g}g^{\mu\nu}=\eta^{\mu\nu}+\psi^{\mu\nu},$$ then the gauge condition $\partial_{\mu}\psi^{\mu\nu}=0$ looks very similar to the well known Lorentz condition (Feynman gauge) $\partial_{\mu}A^{\mu}=0$. If one would like to use the deviation of the covariant metric tensor as a field variable $$g_{\mu\nu}=\eta_{\mu\nu}+h_{\mu\nu},\qquad\left( 2\right)$$ then the weak field expansion of the condition (1) take the form: $$\partial_{\mu}\left( h^{\mu\nu}-\frac{1}{2}\eta^{\mu\nu}h_{\alpha}^{\alpha }\right) =0.$$
The weak-field expansion of the Einstein-Hilbert action with respect to $h_{\mu\nu}$-field (2) has the form: $$S =\frac{1}{16\pi G_{N}}\int\mathrm{d}^{4}x\,\sqrt{-g}\,R\\ =\frac{1}{2\kappa^{2}}\int\mathrm{d}^{4}x\,\left[ \,\partial_{\alpha} h_{\mu\nu}\partial^{\alpha}h^{\mu\nu}-\,\partial_{\alpha}h\,\partial^{\alpha }h-2\,\partial_{\mu}h^{\mu\nu}\left( \partial_{\alpha}h_{\nu}^{\alpha }-\partial_{\nu}h\right) +O\!\left( h^{3}\right) \right] ,$$ where $\kappa=\sqrt{32\pi G_{N}}$. The gauge can be fixed by adding the term: $$\frac{1}{\kappa^{2}}\int\mathrm{d}^{4}x\left( \partial_{\alpha}h_{\mu }^{\alpha}-\frac{1}{2}\partial_{\mu}h\right) \left( \partial_{\beta} h^{\beta\mu}-\frac{1}{2}\partial^{\mu}h\right) ,$$ thus the action takes a particular simple form: $$S=\frac{1}{2\kappa^{2}}\int\mathrm{d}^{4}x\,\left[ \,\partial_{\alpha} h_{\mu\nu}\partial^{\alpha}h^{\mu\nu}-\,\frac{1}{2}\partial_{\alpha }h\,\partial^{\alpha}h+O\!\left( h^{3}\right) \right] .$$ Therefore, in the de Donder gauge the graviton propagator has a very simple form: $$D_{\mu\nu,\alpha\beta}=\left\langle 0\left\vert T\,h_{\mu\nu}\left( x\right) h_{\alpha\beta}\left( y\right) \right\vert 0\right\rangle =i\kappa^{2} \int\frac{\mathrm{d}^{4}p}{\left( 2\pi\right) ^{4}}\frac{e^{-ip\cdot\left( x-y\right) }}{p^{2}+i0}\times\frac{1}{2}\left( \eta_{\mu\alpha}\eta_{\nu\beta }+\eta_{\mu\beta}\eta_{\nu\alpha}-\eta_{\mu\nu}\eta_{\alpha\beta}\right) .$$ The de Donder gauge is so to speak the GR analogue of the Feynman gauge for QCD or QED.
Using the gauge condition (1) and vertices extracted from the weak-field expansion of the Einstein-Hilbert action and utilizing the QFT perturbation theory with respect to $h_{\mu\nu}$, one can find, for example, the gravitational field of a static spinless source. The result will be no more than the $r_{g}/r$-expansion of the Schwarzschild metric in the harmonic coordinates (see, e.g., S. Weinberg, Gravitation and Cosmology, eq. (8.2.15)): $$ds^{2}=\frac{1-r_{g}/\left( 2r\right) }{1+r_{g}/\left( 2r\right) } \,dt^{2}-\frac{1+r_{g}/\left( 2r\right) }{1-r_{g}/\left( 2r\right) }\,\frac{r_{g}^{2}}{4r^{4}}\left( \mathbf{r}\cdot d\mathbf{r}\right) ^{2}-\left( 1+\frac{r_{g}}{2r}\right) ^{2}d\mathbf{r}^{2}.$$