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We explore the possibility that the short-lived radionuclides $^{26}$Al,$^{60}$Fe, $^{107}$Pd, and $^{182}$Hf inferred to be present in the proto-solarcloud originated from $3-8 M_{\odot}$ Asymptotic Giant Branch (AGB) stars.Models of AGB stars with initial mass above 5$M_{\odot}$ are prolific producersof $^{26}$Al owing to hot bottom burning (HBB). In contrast, $^{60}$Fe,$^{107}$Pd, and $^{182}$Hf are produced by neutron captures: $^{107}$Pd and$^{182}$Hf in models $\lesssim 5 M_{\odot}$; and $^{60}$Fe in models withhigher mass. We mix stellar yields from solar-metallicity AGB models into acloud of solar mass and composition to investigate if it is possible to explainthe abundances of the four radioactive nuclides at the Sun's birth using onesingle value of the mixing ratio between the AGB yields and the initial cloudmaterial. We find that AGB stars that experience efficient HBB ($\geq 6M_{\odot}$) cannot provide a solution because they produce too little$^{182}$Hf and $^{107}$Pd relative to $^{26}$Al and $^{60}$Fe. Lower-mass AGBcannot provide a solution because they produce too little $^{26}$Al relative to$^{107}$Pd and $^{182}$Hf. A self-consistent solution may be found for AGBstars with masses in-between ($4-5.5 M_{\odot}$), provided HBB is stronger thanin our models and the $^{13}$C($\alpha$, n)$^{16}$O neutron source is mildlyactivated. If stars of M $< 5.5 M_{\odot}$ are the source of the radioactivenuclides, then some basis for their existence in proto-solar clouds needs to beexplored, given that the stellar lifetimes are longer than the molecular cloudlifetimes.

Intermediate-mass asymptotic giant branch stars and sources of $^{26}$Al, $^{60}$Fe, $^{107}$Pd, and $^{182}$Hf in the solar system