  The composition of the most primitive Solar System condensates, such as
calcium-aluminum-rich inclusions (CAI) and micron-sized corundum grains, show
that short-lived radionuclides (SLR), e.g., 26Al, were present in the early
Solar System. Their abundances require a local origin, which however is far
from being understood. We present for the first time the abundances of several
SLR up to 60Fe predicted from stars with initial mass in the range roughly 7-11
Msun. These stars evolve through core H, He, and C burning. After core C
burning they go through a "Super"-asymptotic giant branch (Super-AGB) phase,
with the H and He shells activated alternately, episodic thermal pulses in the
He shell, a very hot temperature at the base of the convective envelope (~ 10^8
K), and strong stellar winds driving the H-rich envelope into the surrounding
interstellar medium. The final remnants of the evolution of Super-AGB stars are
mostly O-Ne white dwarfs. Our Super-AGB models produce 26Al/27Al yield ratios ~
0.02 - 0.26. These models can account for the canonical value of the 26Al/27Al
ratio using dilutions with the Solar Nebula of the order of 1 part of Super-AGB
mass per several 10^2 to several 10^3 of Solar Nebula mass, resulting in
associated changes in the O composition in the range 3 permil to 20 permil.
This is in agreement with observations of the O isotopic ratios in primitive
Solar System condensated, which do not carry the signature of a stellar
pollutor. The radionuclides 41Ca and 60Fe are produced by neutron captures in
Super-AGB stars and their meteoritic abundances are also matched by some of our
models, depending on the nuclear and stellar physics uncertainties as well as
the meteoritic experimental data. We also expect and are currently
investigating Super-AGB production of SLR heavier than iron, such as 107Pd.

Solar and Stellar Astrophysics