We present results on the ability of microturbulence, LTE line formation, and a homogeneous thermal model to realistically represent the center-limb variation of temporally and spacially averaged solar line profiles. We have used three somewhat similar semi-empirical thermal models in combination with five current microturbulence models which cover the gamut of homogeneous-isotropic to nonhomogeneous-anisotropic. From high resolution photoelectric data for λ λ5000–6000 at five μ-values (1, 0.63, 0.4, 0.25, 0.16) obtained at KPNO, we selected 17 Fe i and 5 Fe ii line profiles to unblend and symmetrize for study. An iterative scheme has been developed to calculate theoretical profiles for the various combination of models and compare them to the observed profile using the abundance at each limb position and the magnitude of the pressure broadening at the center of the disc as parameters. We find that a microturbulence model, for which the radial and tangential components increase into deeper layers with ξtan>ξrad, produces a reasonable good center-limb fit for lines less than 100 mA. However, for lines stronger than 140 mA, microturbulence models with no depth dependence produce the best match between theory and observation. Thus, there is reason to question the uniqueness of the microturbulence concept.