  Short-lived radionuclides, such as 26Al and 60Fe, are tracers of star
formation. Therefore, their abundances can unravel the recent star formation
history of the host galaxy. In view of future gamma-ray surveys, we predict the
masses and fluxes of these two elements in the Large Magellanic Cloud (LMC)
using new chemical evolution models. Our best model reproduces the abundance
patterns of alpha/Fe ratios, the gas mass, the average metallicity, the present
time supernova and nova rates observed in LMC. We show three main results: i)
the best model for the LMC suggests a star formation rate very mild at the
beginning with a recent burst, and a Salpeter-like initial mass function. ii)
The predicted mass of 26Al is 0.33 M_Sun, 2/3 produced by massive stars and 1/3
by novae. iii) The predicted mass of 60Fe is 0.44 M_Sun, entirely produced by
massive stars. This result suggests a larger fraction of 60Fe, at variance with
the Milky Way. The explanation for this lies in the adopted initial mass
function, that for the LMC contains more massive stars than for the Milky Way.
These predictions can be useful for the COSI-SMEX mission planned for launch in
2027. The expected gamma-ray line fluxes for the 1.809 MeV line of 26Al and the
1.173 and 1.332 MeV lines of 60Fe are in the range of (0.2-2.7)x10^-6 ph cm^-2
s^-1 and (0.7-2.8)x10^-7 ph cm^-2 s^-1, respectively. This new instrument could
have the sensitivity to detect the upper end of the predicted 1.8 MeV flux
within its nominal two-year mission.
