Dust destruction in non-radiative shocks
  Supernova remnant (SNR) shock waves are the main place where interstellar
dust grains are destroyed. However, the dust destruction efficiency in
non-radiative shocks is still not well known. One way to estimate the fraction
of dust destroyed is to compare the difference between postshock gas abundances
and preshock medium total abundances when the preshock elemental depletion
factors are known. We compare the postshock gas abundances of 16 SNRs in Large
Magellanic Cloud (LMC) with the LMC interstellar medium abundances that we
derived based on 69 slow-rotating early B-type stars. We find that, on average,
$\sim$61\% of Si rich dust grains are destroyed in the shock while the fraction
of dust destroyed is only $\sim$40\% for Fe rich dust grains. This result
supports the idea that the high depletion of Fe in the diffuse neutral medium
is not caused by the resilience of Fe rich grains but because of faster growth
rate. This work also presents a potential way to constrain the chemical
composition of interstellar dust.
