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The formation and chemical evolution of the Milky Way Galaxy is numericallysimulated by developing a Monte Carlo approach to predict the elementalabundance gradients and other galactic features using the revised solarabundance. The galaxy is accreted gradually by using either a two-infall or athree-infall accretion scenario. The galaxy is chemically enriched by thenucleosynthetic contributions from an evolving ensemble of generations ofstars. We analyse the role of star formation efficiency. The influence of theradial gas inflow as well as radial gas mixing on the evolution of galaxy isalso studied. The SN Ia delay time distribution (DTD) is incorporated bysynthesizing SN Ia populations using random numbers based on a distributionfunction. The elemental abundance evolutionary trends corroborate fractionalcontributions of ~0.1 from prompt ( < 100 Myr) SN Ia population. The modelspredict steep gradients in the inner regions and less steep gradients in theouter regions which agrees with the observations. The gradients indicate anaverage radial gas mixing velocity of < 1 km/s. The models with radial gasinflows reproduce the observed inversion in the elemental abundance gradientsaround 2 billion years. The three-infall accretion scenario performs betterthan the two-infall accretion model in terms of explaining the elementalabundance distributions of the galactic halo, thick and thin discs. Theaccuracy of all the models has been monitored as a cumulative error of < 0.15 Min the mass balance calculations during the entire evolution of the galaxy.

A Monte Carlo based simulation of the galactic chemical evolution of the Milky Way galaxy