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tokens: Because complete atomic line lists for these heavy species are not available (Kasen et al. 2013 ), we have simply assumed that the energy integral of the full radiative spectra of r -process material is similar to that of Fe. Under these conditions, we find that metal cooling from r -process material is not expected to influence the dynamics of NSBM remnants expanding into an ambient medium with . The resulting NSBM remnant evolution in these environments should solely be determined by the metal cooling of the swept-up material. However, the mass fraction of r -process material at shell formation within the remnant is expected to be severely enhanced to about , assuming a solar abundance ratio and . In contrast, with a total r -process mass per supernova of (Shen et al. 2015 ), we expect a local enhancement of only about when a Type II SNR attains shell formation in similar external conditions. Of particular relevance in this case is the heavy element composition of galactic halo stars with the metallicity regime , which has been found to have pure r -process products with a distribution that is characteristic of solar system matter but with a large star-to-star scatter in their r -process concentrations (Sneden et al. 2008 ). In some stars with , the r -process enrichment can be as large as 10 2 , assuming a solar abundance ratio. The presence of r -process material in these stars with a distribution that is characteristic of solar abundance ratios illustrates that r -process enrichment has operated in a fairly robust manner, while their abundance dispersions further suggest that r -process production sites must be rare and locally very enhanced, as expected from NSBM enrichment (e.g., Shen et al. 2015 ). These localized inhomogeneities would then be smoothed out as more NSBMs take place and r -process material is given more time to be transported and mixed throughout the early Milky Way. Metal feedback from NSBM remnants is thus essential to understand the formation of r -process enhanced stars in galaxies. Despite the initial differences, our conclusions regarding the efficacy of the transport and mixing of r -process material by NSBM remnants in a cosmological context should be similar to that expected from single SNRs. APPENDIX RESOLUTION CONVERGENCE Here we describe the results of our resolution study. Simulations are initialized with a static AMR and with a maximum level of refinement of 10 within a sphere enclosing all of the tail material. In all cases, we reduce the refinement by two levels after the size of the tidal remnant reaches 1/20 of the size of the computational box. The grid mesh refinement is then based on the value of the density. To test how our results are sensitive to the refinement criteria and resolution, we run two more simulations using the initial fiducial model parameters but subtracting three and one level(s) of refinement, respectively. We compare the different simulations in Figure 8 with final