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The early solar system contained a short-lived radionuclide, 26Al (its half-life time t1／2 = 0.7 Myr). The decay energy 26Al is thought to have controlled thermal evolution of planetesimals and, possibly, the water contents of planets. Mmany hypotheses have been proposed for the origin of 26Al in the solar system. One of the possible hypotheses is the ‘disk injection scenario’; when the protoplanetary disk of the solar system had already formed, a nearby (< 1 pc) supernova (SN) injected radioactive material directly into the disk. Such a 26Al injection hypothesis has been tested so far with limited setups for disk structure and SN distance. Moreover, a nearby SN could disrupt a disk, but disruption and injection conditions have been considered separately. Here we revisit this problem to investigate whether there are self-consistent conditions under which the surviving disk radius can receive enough 26Al which can account for the abundance in the early solar system. We also consider a range of disk mass and structure, 26Al yields from SN, and large dust mass fraction ηd. We find that 26Al yields of SN are required as ≳ 2.1 × 10−3M⊙(ηd/0.2)−1, which is difficult to reproduce given the possible range of ejected 26Al mass and large dust mass fractions from the supernovae. Furthermore, we find that even if the above conditions are met, the SN shock changes the disk temperature, which may not be consistent with the solar-system record. Our results place a strong constraint on the disk injection scenario. Rather, we suggest that the fresh 26Al of the early solar system must have been synthesized/injected in other ways.