Microturbulence ( ξ ) is a key parameter introduced in stellar spectroscopy to explain the strength of saturated lines by formally incorporating an additional thermal broadening term in the line opacity profile. Although our Sun can serve as an important testing bench to check the usual assumption of constant ξ , the detailed behavior of how ξ varies from the disk center through the limb seems to have never been investigated so far. In order to fill this gap, local ξ values on the solar disk were determined from the equivalent widths of 46 Fe  i lines at 32 points from the center to the limb by requiring the consistency between the abundances derived from lines of various strengths. The run of ξ with θ (angle between the line of sight and the surface normal) was found to be only gradual from ≈ 1.0 km s −1 (at sin θ = 0 : disk center) to ≈ 1.3 km s −1 (at sin θ ≈ 0.7 : two-thirds of radial distance); but thereafter increasing more steeply up to ≈ 2 km s −1 (at sin θ = 0.97 : limb). This result further suggests that the microturbulence derived from the flux spectrum of the disk-integrated Sun is ≈ 20 % larger than that of the disk-center value, which is almost consistent with the prediction from 3D hydrodynamical model atmospheres.