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Most studies suggest the pollution of white dwarf (WD) atmospheres arisesfrom accretion of minor planets, but the exact properties of pollutingmaterial, and in particular the evidence for water in some cases are not yetunderstood. Here we study the water retention of small icy bodies in exo-solarplanetary systems, as their respective host stars evolve through and off themain sequence and eventually become WDs. We explore for the first time a widerange of star masses and metallicities. We find that the mass of the WDprogenitor star is of crucial importance for the retention of water, while itsmetallicity is relatively unimportant. We predict that minor planets aroundlower-mass WD progenitors would retain more water in general, and would do soat closer distances from the WD, compared with high-mass progenitors. Thedependence of water retention on progenitor mass and other parameters hasdirect implications for the origin of observed WD pollution, and we discuss howour results and predictions might be tested in the future as more observationsof WDs with long cooling-ages become available.

Post main sequence evolution of icy minor planets II: water retention and white dwarf pollution around massive progenitor stars