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We have developed a numerical galactic chemical evolution model. The model isconstructed such that the effect of a wide range of parameters can beinvestigated. It takes into account results from stellar evolution models, adifferentiation between diverse types of core collapse SNe and the contributionof AGB stars in the mass range 3-8 Msun. We consider the lifetime-dependentyield injection into the ISM by all sources as well as dust destruction due toSN shocks in the ISM. We ascertain the temporal progression of the dust mass,the dust-to-gas and dust-to-metal mass ratios as well as other physicalproperties of a galaxy and study their dependence on the mass of the galaxy,the IMF, dust production efficiencies and dust destruction in the ISM. Theamount of dust and the physical properties of a galaxy strongly depend on theinitial gas mass available. Overall, while the total amount of dust producedincreases with galaxy mass, the detailed outcome depends on the SN dustproduction efficiency, the IMF and the strength of dust destruction in the ISM.Dust masses are higher for IMFs biased towards higher stellar masses, despitethe fact that these IMFs are more strongly affected by dust destruction in theISM. The sensitivity to the IMF increases as the mass of the galaxy decreases.SNe are primarily responsible for a significant enrichment with dust at earlyepochs (< 200 Myr). Dust production with a dominant contribution by AGB starsis found to be insufficient to account for dust masses in excess of 10^8 Msunwithin 400 Myr after starburst. We find that galaxies with initial gas massesbetween 1-5 x 10^11 Msun are sufficiently massive to enable production of dustmasses >10^8 Msun. Our preferred scenario is dominated by SN dust production incombination with top-heavy IMFs and moderate dust destruction in the ISM.

Genesis and evolution of dust in galaxies in the early Universe I. Modeling dust evolution in starburst galaxies