  The early solar system contained a short-lived radionuclide, $^{26}$Al (its
half-life time $t_{1/2} = 0.7$ Myr). The decay energy $^{26}$Al 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
$^{26}$Al 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 $(<1 \,\mathrm{pc})$ supernova injected radioactive
material directly into the disk. Such a $^{26}$Al injection hypothesis has been
tested so far with limited setups for disk structure and supernova distance,
and treated disk disruption and $^{26}$Al injection separately. Here, we
revisit this problem to investigate whether there are self-consistent
conditions under which the surviving disk radius can receive enough $^{26}$Al
which can account for the abundance in the early solar system. We also consider
a range of disk mass and structure, $^{26}$Al yields from supernova, and a
large dust mass fraction $\eta_\mathrm{d}$. We find that $^{26}$Al yields of
supernova are required as $\gtrsim
2.1\times10^{-3}M_\odot(\eta_\mathrm{d}/0.2)^{-1}$, challenging to achieve with
known possible $^{26}$Al 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 $^{26}$Al of the early solar system must have been
synthesized/injected in other ways.
