Wave equation given a cosmological inflationary metric

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To derive the wave equation from the given cosmological inflationary metric, one must apply Einstein's equations alongside the stress-energy tensor of the scalar field. The specific metric provided leads to the relation involving the scalar field, which is expressed as a function of time. By substituting this metric into the equations, one can arrive at a form that resembles a Bessel's equation. Understanding the transformation steps is crucial for grasping how the wave equation evolves from the metric. This process highlights the interplay between geometry and field dynamics in cosmological contexts.
Nick2014
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Hi everybody!
Can you explain me how I can obtain wave equation given a metric? For example, if I have this metric $$g_{μν}=diag(−e^{2a(t)},e^{2b(t)},e^{2b(t)},e^{2b(t)})$$, how can derive the relation $$\frac{1}{\sqrt{g}}\partial _t(g^{00}\sqrt{g}\partial _t \phi)+\frac{1}{\sqrt{g}}g^{ii}\partial ^2 \phi$$ where ##\phi=\phi (t)## is a scalar field? Moreover, from this equation the professor has derived a Bessel's equation in the form u¨+ταu=0. I don't understand... Thanks
 
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You'd need to use Einstein's equations with the stress-energy tensor of the scalar field on the right hand side.
 
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Chalnoth said:
You'd need to use Einstein's equations with the stress-energy tensor of the scalar field on the right hand side.

And then, to obtain that relation?
 
That will give you the relation you've written down in your post. To get the Bessel equation, simply substitute in the metric you've been provided.
 
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OK, thanks :)
 
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https://en.wikipedia.org/wiki/Recombination_(cosmology) Was a matter density right after the decoupling low enough to consider the vacuum as the actual vacuum, and not the medium through which the light propagates with the speed lower than ##({\epsilon_0\mu_0})^{-1/2}##? I'm asking this in context of the calculation of the observable universe radius, where the time integral of the inverse of the scale factor is multiplied by the constant speed of light ##c##.
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