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This common belief is wrong as the requirements for only the inside the sphere to govern the dynamics are not satisfied. The requirement is that the boundary conditions at infinity do not spoil the symmetry - which is true when you consider a potential that tends to zero at infinity. However, the Poisson equation with a constant density term is incompatible with any solution where the symmetry is maintained. This implies external fields - givenby the boundary conditions - also exist inside the sphere. Compare with adding an external electric field to the field of a soherical charge distribution. The external field will certainly affect the dynamics of a test charge inside the sphere.kimbyd said:A homogeneous and isotropic universe is spherically-symmetric, at every location. We know from that symmetry and Gauss's Law that whatever sphere of the Universe we're looking at at any given time, the behavior of the system outside has no impact on the dynamics inside the sphere. From this we get a result which states how the density of that sphere will change over time. Since we could have used any origin and any size sphere to get this result, it applies to the entire universe.
Will Learn said:I can only point to the lectures that are available online from Leonard Susskind. In those Cosmology lectures, the Friedmann equations were derived entirely using Newtonian physics. GR was only used at the very end and just to show that the same equations appear. I think @kimbyd has made this point.
The ability to derive the Friedmann equations from Newtonian physics may be a little surprising but it's not unlike the derivation of an object that was called a "dark star" and has many of the same properties for the object we now describe as a Black hole using GR.
Those are usually heuristic arguments. Regardless, it is not the same Friedmann equation as it is based on Newtonian physics. There is no a priori reason to expect the exact same result in a FLRW universe.