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We update an existing code that treats the destruction of dust in supernova-triggered shock waves, introducing more physics and new features in order to arrive at a more realistic modelling of dust processing in shock waves. We follow the evolution of the dust size distribution along the shock and calculate the dust emission after the shock. Finally, co mparing the pre-shock and post-shock distributions, we estimate the integrated dust destructio n and lifetime in our Galaxy. We find that both carbonaceous and silicate grain lifetimes are sho rt compared to the timescale of their formation around evolved stars (stardust), thus affirming t he long-standing conclusion that dust must be re-formed in the denser regions of the ISM.

Dust Lifetime Re-evaluation in the Light of a New Dust Model