We present MIRI/JWST medium-resolution spectroscopy (MRS) and imaging (MIRIM) of the lensed galaxy MACS1149-JD1 at a redshift of \(z\)=9.1092\(\pm\)0.0002 (Universe age about 530 Myr). We detect, for the first time, spatially resolved H\(\alpha\) emission in a galaxy at a redshift above nine. The structure of the H\(\alpha\) emitting gas consists of two clumps, S and N. The total H\(\alpha\) luminosity implies an instantaneous star-formation of 5.3\(\pm\)0.4 \(M_{\odot}\) yr\(^{-1}\) for solar metallicities. The ionizing photon production efficiency, \(\log(\zeta_\mathrm{ion})\), shows a spatially resolved structure with values of 25.55\(\pm\)0.03, 25.47\(\pm\)0.03, and 25.91\(\pm\)0.09 Hz erg\(^{-1}\) for the integrated galaxy, and clumps S and N, respectively. The H\(\alpha\) rest-frame equivalent width, EW\(_{0}\)(H\(\alpha\)), is 726\(^{+660}_{-182}\) Ángstrom for the integrated galaxy, but presents extreme values of 531\(^{+300}_{-96}\) Ángstrom and \(\geq\)1951 Ángstrom for clumps S and N, respectively. The spatially resolved ionizing photon production efficiency is within the range of values measured in galaxies at redshift above six, and well above the canonical value (25.2\(\pm\)0.1 Hz erg\(^{-1}\)). The extreme difference of EW\(_{0}\)(H\(\alpha\)) for Clumps S and N indicates the presence of a recent (<5 Myrs) burst in clump N and a star formation over a larger period of time (e.g., \(\sim\)50 Myr) in clump S. Finally, clump S and N show very different H\(\alpha\) kinematics with velocity dispersions of 56\(\pm\)4 km s\(^{-1}\) and 113\(\pm\)33 km s\(^{-1}\), likely indicating the presence of outflows or increased turbulence in the clump N. The dynamical mass, \(M_\mathrm{dyn}\)= (2.4\(\pm\)0.5)\(\times\)10\(^{9}\) \(M_{\odot}\), is within the range measured with the spatially resolved OIII88\(\mu\)m line.