Fig. 2.
Radial profile of the dust mass surface density for M 101 (top), NGC 628 (middle), and M 33 (bottom) compared to the profiles provided by the simulations performed by Aoyama et al. (2017) and Hou et al. (2017). Dust production in stellar ejecta, dust destruction by SN shocks, grain growth by accretion and coagulation, as well as shattering, are taking into account in the simulations.
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