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We present evolutionary calculations for the size and aromatization degreedistributions of interstellar dust grains, driven by their destruction byradiation, collisions with gas particles, and shattering due to grain-graincollisions. Based on these calculations we model dust emission spectra. Theinitial grain size distribution play the important role in the evolution of anensemble of dust particles. Radiation in the considered intensity range mostlyaromatizes grains. The smallest grains are mainly destructed via sputtering bycollisions with gas particles. There are no grains smaller than 20~\AA\ in themedium at relative gas-dust velocities more than 50~km/s, which is typical forshocks in supernova remnants. The IR emission spectrum changes significantlydue to the dust evolution depending on the adopted grain properties, inparticular, on the energy of the C--C bonds ($E_0$). Aromatic bands in thenear-IR (2--15~$\mu$m) are absent, if $E_0$ is low, even when the mediumproperties correspond to the average interstellar medium in our Galaxy. As inreality these bands are observed, high $E_0$ values are more preferable. Weconsider dependence of the emission intensity ratios for various photometricbands on the medium properties. The aromatization degree of small grains showsup most strongly in the $I_{3.4}/I_{11.3}$ intensity ratio while the fractionof aromatic grains in the total dust mass influences the $I_{3.3}/I_{70+160}$ratio.

The evolution of hydrocarbon dust grains in the interstellar medium and its influence on the infrared spectra of dust