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We present a physically-motivated model involving the different processesaffecting supernova dust grains as they are incorporated into the thermalizedmedium within young massive star clusters. The model is used to explain thenear- to mid-infrared (NIR-MIR) excess found in such clusters and usuallymodeled as a blackbody with temperature $\sim (400-1000)$ K. In our approach,dust grains are efficiently produced in the clumpy ejecta of core-collapsesupernovae, fragmented into small pieces ($\lesssim 0.05$ $\mu$m) as they areincorporated into the hot and dense ISM, heated via frequent collisions withelectrons and the absorption of energetic photons. Grains with small sizes canmore easily acquire the high temperatures ($\sim 1000$ K) required to produce aNIR-MIR excess with respect to the emission of foreground PAHs and starlight.However, the extreme conditions inside young massive clusters make difficultfor these small grains to have a persistent manifestation at NIR-MIRwavelengths as they are destroyed by efficient thermal sputtering.Nevertheless, the chances for a persistent manifestation are increased bytaking into account that small grains become increasingly transparent to theirimpinging ions as their size decreases. For an individual SN event, we findthat the NIR-MIR excess last longer if the time required to incorporate all thegrains into the thermalized medium is also longer, and in some cases,comparable to the characteristic interval between supernova explosions. Ourmodels, can successfully explain the near-infrared excesses found in the starclusters observed in M33 (Rela\~no et al. 2016) assuming a low heatingefficiency and mass-loading. In this scenario, the presence of the NIR-MIRexcess is an indication of efficient dust production in SNe and its subsequentdestruction

Can Dust Injected by SNe Explain the NIR-MIR Excess in Young Massive Stellar Clusters?