Star formation is one of the key factors that shapes galaxies. This process is relatively well understood from both simulations and observations on a small local scale of individual giant molecular clouds and also on a global galaxy-wide scale (e.g. the Kennicutt-Schmidt law). However, there is still no understanding on how to connect global to local star formation scales and whether this connection is at all possible. Here we analyze spatially resolved kinematics and the star formation rate density $Sigma_{SFR}$ for a combined sample of 17 nearby spiral galaxies obtained using our own optical observations in H$alpha$ for 9 galaxies and neutral hydrogen radio observations combined with a multi-wavelength spectral energy distribution analysis for 8 galaxies from the THINGS project. We show that the azimuthally averaged normalized star formation rate density in spiral galaxies on a scale of a few hundred parsecs is proportional to the kinetic energy of giant molecular cloud collisions due to differential rotation of the galactic disc. This energy is calculated from the rotation curve using the two Oort parameters A and B as $log (Sigma_{SFR} / SFR_{tot}) propto log[2 A^2+ 5 B^2]$. The total kinetic energy of collision is defined by the shear velocity that is proportional to A and the rotational energy of a cloud proportional to the vorticity B. Hence, shear does not act as a stabilizing factor for the cloud collapse thus reducing star formation but rather increases it by boosting the kinetic energy of collisions. This result can be a tool through which one can predict a radial distribution of star formation surface density using only a rotation curve.
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