When I see harmonic coordinates used somewhere, what should my association be?
Is there some general use or need to consider the harmonic coordinate 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 understand their significance, other than that one can consequently algebraically use the relation Δxμ=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 coordinates have some special role in geometric quantization?
Answer
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: DμAμ→gμν∂μAν,gμνDνDμϕ→gμν∂μ∂νϕ. The harmonic condition ∂μ(√−ggμν)=0(1) is widely used to construct the so called de Donder gauge for the quantization of a weak gravitational field. If one uses the deviation ψμν of the contravariant metric density from the flat one ημν=diag(1,−1,−1,−1) as a field variable: √−ggμν=ημν+ψμν, then the gauge condition ∂μψμν=0 looks very similar to the well known Lorentz condition (Feynman gauge) ∂μAμ=0. If one would like to use the deviation of the covariant metric tensor as a field variable gμν=ημν+hμν,(2) then the weak field expansion of the condition (1) take the form: ∂μ(hμν−12ημνhαα)=0.
The weak-field expansion of the Einstein-Hilbert action with respect to hμν-field (2) has the form: S=116πGN∫d4x√−gR=12κ2∫d4x[∂αhμν∂αhμν−∂αh∂αh−2∂μhμν(∂αhαν−∂νh)+O(h3)], where κ=√32πGN. The gauge can be fixed by adding the term: 1κ2∫d4x(∂αhαμ−12∂μh)(∂βhβμ−12∂μh), thus the action takes a particular simple form: S=12κ2∫d4x[∂αhμν∂αhμν−12∂αh∂αh+O(h3)]. Therefore, in the de Donder gauge the graviton propagator has a very simple form: Dμν,αβ=⟨0|Thμν(x)hαβ(y)|0⟩=iκ2∫d4p(2π)4e−ip⋅(x−y)p2+i0×12(ημαηνβ+ημβηνα−ημνηαβ). 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 hμν, one can find, for example, the gravitational field of a static spinless source. The result will be no more than the rg/r-expansion of the Schwarzschild metric in the harmonic coordinates (see, e.g., S. Weinberg, Gravitation and Cosmology, eq. (8.2.15)): ds2=1−rg/(2r)1+rg/(2r)dt2−1+rg/(2r)1−rg/(2r)r2g4r4(r⋅dr)2−(1+rg2r)2dr2.
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