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We use N-body simulations of star cluster evolution to explore the hypothesisthat short-lived radioactive isotopes found in meteorites, such as 26-Al, weredelivered to the Sun's protoplanetary disc from a supernova at the epoch ofSolar System formation. We cover a range of star cluster formation parameterspace and model both clusters with primordial substructure, and those withsmooth profiles. We also adopt different initial virial ratios - from cool,collapsing clusters to warm, expanding associations. In each cluster we placethe same stellar population; the clusters each have 2100 stars, and contain onemassive 25M_Sun star which is expected to explode as a supernova at about6.6Myr. We determine the number of Solar (G)-type stars that are within 0.1 -0.3pc of the 25M_Sun star at the time of the supernova, which is the distancerequired to enrich the protoplanetary disc with the 26-Al abundances found inmeteorites. We then determine how many of these G-dwarfs are unperturbed`singletons'; stars which are never in close binaries, nor suffer sub-100auencounters, and which also do not suffer strong dynamical perturbations.  The evolution of a suite of twenty initially identical clusters is highlystochastic, with the supernova enriching over 10 G-dwarfs in some clusters, andnone at all in others. Typically only ~25 per cent of clusters containenriched, unperturbed singletons, and usually only 1 - 2 per cluster (from atotal of 96 G-dwarfs in each cluster). The initial conditions for starformation do not strongly affect the results, although a higher fraction ofsupervirial (expanding) clusters would contain enriched G-dwarfs if thesupernova occurred earlier than 6.6Myr. If we sum together simulations withidentical initial conditions, then ~1 per cent of all G-dwarfs in oursimulations are enriched, unperturbed singletons.

Supernova enrichment and dynamical histories of solar-type stars in clusters