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It has been speculated that WR winds may have contaminated the forming solarsystem, in particular with short-lived radionuclides (half-lives in theapproximate 10^5 - 10^8 y range) that are responsible for a class of isotopicanomalies found in some meteoritic materials. We revisit the capability of theWR winds to eject these radionuclides using new models of single non-explodingWR stars with metallicity Z = 0.02. The earlier predictions for non-rotating WRstars are updated, and models for rotating such stars are used for the firsttime in this context. We find that (1) rotation has no significant influence onthe short-lived radionuclide production by neutron capture during the coreHe-burning phase, and (2) 26Al, 36Cl, 41Ca, and 107Pd can be wind-ejected by avariety of WR stars at relative levels that are compatible with the meteoriticanalyses for a period of free decay of around 10^5 y between production andincorporation into the forming solar system solid bodies. We confirm thepreviously published conclusions that the winds of WR stars have a radionuclidecomposition that can meet the necessary condition for them to be a possiblecontaminating agent of the forming solar system. Still, it remains to bedemonstrated from detailed models that this is a sufficient condition for thesewinds to have provided a level of pollution that is compatible with theobservations.Comment: 8 pages, 8 figure

The production of short-lived radionuclides by new non-rotating and rotating Wolf-Rayet model stars