  Aluminium-26 is a radioactive isotope which can be synthesized within
asymptotic giant branch (AGB) stars, primarily through hot bottom burning.
Studies exploring $^{26}$Al production within AGB stars typically focus on
single-stars; however, observations show that low- and intermediate-mass stars
commonly exist in binaries. We use the binary population synthesis code
binary_c to explore the impact of binary evolution on $^{26}$Al yields at solar
metallicity both within individual AGB stars and a low/intermediate-mass
stellar population. We find the key stellar structural condition achieving most
$^{26}$Al overproduction is for stars to enter the thermally-pulsing AGB
(TP-AGB) phase with small cores relative to their total masses, allowing those
stars to spend abnormally long times on the TP-AGB compared to single-stars of
identical mass. Our population with a binary fraction of 0.75 has an $^{26}$Al
weighted population yield increase of $25\%$ compared to our population of only
single-stars. Stellar-models calculated from the Mt Stromlo/Monash Stellar
Structure Program, which we use to test our results from binary_c and closely
examine the interior structure of the overproducing stars, support our binary_c
results only when the stellar envelope gains mass after core-He depletion.
Stars which gain mass before core-He depletion still overproduce $^{26}$Al, but
to a lesser extent. This introduces some physical uncertainty into our
conclusions as $55\%$ of our $^{26}$Al overproducing stars gain envelope mass
through stellar wind accretion onto pre-AGB objects. Our work highlights the
need to consider binary influence on the production of $^{26}$Al.
