Map of the formation region of planetesimals as a function of time. The position of the water ice line and the silicate sublimation line (1350 K) are calculated from the dead zone model of Johansen et al. (2021) that considers stellar irradiation as well as viscous heating where the thermal ionization level is above the threshold for the magnetoro-tational instability. We assumed here a basic ²⁶Al/²⁷Al of 0.25 times the value in the CAI-forming region (Larsen et al. 2011; Connelly et al. 2012). Exterior of the water ice line, FeO-rich bodies form when the formation time is early enough to melt the ice. Differentiated and primitive FeO-poor bodies form interior of the water ice line, perhaps analogues of the enstatite chondrites.