Core-collapse supernovae can condense large masses of dust post-explosion .
However , sputtering and grain-grain collisions during the subsequent passage of the dust through the reverse shock can potentially destroy a significant fraction of the newly formed dust before it can reach the interstellar medium .
Here we show that in oxygen-rich supernova remnants like Cassiopeia A the penetration and trapping within silicate grains of the same impinging ions of oxygen , silicon and magnesium that are responsible for grain surface sputtering can significantly reduce the net loss of grain material .
We model conditions representative of dusty clumps ( density contrast \chi = 100 ) passing through the reverse shock in the oxygen-rich Cassiopeia A remnant and find that , compared to cases where the effect is neglected , as well as facilitating the formation of grains larger than those that had originally condensed , ion trapping increases the surviving masses of silicate dust by factors of up to two to four , depending on initial grain radii .
For higher density contrasts ( \chi \gtrsim 180 ) , we find that the effect of gas accretion on the surface of dust grains surpasses ion trapping , and the survival rate increases to { \sim } 55 \mathrm { \% } of the initial dust mass for \chi = 256 .