  The presence of short-lived radioisotopes (SLRs) 26-Al and 60-Fe in the Solar
system places constraints on the initial conditions of our planetary system.
Most theories posit that the origin of 26-Al and 60-Fe is in the interiors of
massive stars, and they are either delivered directly to the protosolar disc
from the winds and supernovae of the massive stars, or indirectly via a
sequential star formation event. However, massive stars that produce SLRs also
emit photoionising far and extreme ultraviolet radiation, which can destroy the
gas component of protoplanetary discs, possibly precluding the formation of gas
giant planets like Jupiter and Saturn. Here, we perfom N-body simulations of
star-forming regions and determine whether discs that are enriched in SLRs can
retain enough gas to form Jovian planets. We find that discs are enriched and
survive the photoionising radiation only when the dust radius of the disc is
fixed and not allowed to move inwards due to the photoevaporation, or outwards
due to viscous spreading. Even in this optimal scenario, not enough discs
survive until the supernovae of the massive stars and so have zero or very
little enrichment in 60-Fe. We therefore suggest that the delivery of SLRs to
the Solar system may not come from the winds and supernovae of massive stars.
