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We investigate the time evolution of dust properties, molecular hydrogen(H_2) contents, and star formation histories in galaxies by using our originalchemodynamical simulations. The simulations include the formation of dust inthe stellar winds of supernovae (SNe) and asymptotic giant branch (AGB) stars,the growth and destruction processes of dust in the interstellar medium (ISM),the formation of polycyclic aromatic hydrocarbon (PAH) dust in carbon-rich AGBstars, the H_2 formation on dust grains, and the H_2 photo-dissociation due tofar ultra-violet (FUV) light in a self-consistent manner. We focus mainly ondisk galaxies with different total masses in this preliminary study. Theprinciple results are as follows: The star formation histories of disk galaxiescan be regulated by the time evolution of interstellar dust, mainly because theformation rates of H_2 can be controlled by dust properties. The observedcorrelation between dust-to-gas-ratios (D) and gas-phase oxygen abundances (A_O= 12+log(O/H)) can be reproduced reasonably well in the present models. Thedisks show negative radial gradients (i.e., larger in inner regions) of H_2fraction (f_H2), PAH-to-dust mass ratio (f_PAH), D, and A_O and these gradientsevolve with time. The surface-mass densities of dust (Sigma_dust) arecorrelated more strongly with the total surface gas densities than with thoseof H_2. Local gaseous regions with higher D are more likely to have higher f_H2in individual disks and total H_2 masses correlate well with total dust masses.More massive disk galaxies are more likely to have higher D, f_PAH, and f_H2and smaller dust-to-stellar mass ratios. We also compare between galactic starformation histories in the metallicity-dependent and dust-dependent starformation models and find no major differences.

Coevolution of dust, gas, and stars in galaxies - I. Spatial distributions and scaling-relations of dust and molecular hydrogen