Self-consistent Conditions for 26Al Injection into a Protosolar Disk from a Nearby Supernova

The early solar system contained a short-lived radionuclide, Al-26 (its half-life time t(1/2) = 0.7 Myr). The decay energy of Al-26 is thought to have controlled the thermal evolution of planetesimals and, possibly, the water contents of planets. Many hypotheses have been proposed for the origin of Al-26 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 injected radioactive material directly into the disk. Such a Al-26 injection hypothesis has been tested so far with limited setups for disk structure and supernova distance, which have treated disk disruption and Al-26 injection separately. Here, we revisit this problem, to investigate whether there are self-consistent conditions under which the surviving disk radius can receive enough Al-26 to account for the abundance in the early solar system. We also consider a range of disk masses and structures, Al-26 yields from supernova, and a large dust mass fraction eta d. We find that Al-26 yields of supernova are required as greater than or similar to 2.1x10(-3)M(circle dot)(eta d/0.2)(-1) , which are challenging to achieve with the known possible Al-26 ejection and dust mass fraction ranges. Furthermore, we find that even if the above conditions are met, the supernova flow 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 Al-26 of the early solar system must have been synthesized/injected in other ways.