A Monte Carlo based simulation of the galactic chemical evolution of the
  Milky Way galaxy
  The formation and chemical evolution of the Milky Way Galaxy is numerically
simulated by developing a Monte Carlo approach to predict the elemental
abundance gradients and other galactic features using the revised solar
abundance. The galaxy is accreted gradually by using either a two-infall or a
three-infall accretion scenario. The galaxy is chemically enriched by the
nucleosynthetic contributions from an evolving ensemble of generations of
stars. We analyse the role of star formation efficiency. The influence of the
radial gas inflow as well as radial gas mixing on the evolution of galaxy is
also studied. The SN Ia delay time distribution (DTD) is incorporated by
synthesizing SN Ia populations using random numbers based on a distribution
function. The elemental abundance evolutionary trends corroborate fractional
contributions of ~0.1 from prompt ( < 100 Myr) SN Ia population. The models
predict steep gradients in the inner regions and less steep gradients in the
outer regions which agrees with the observations. The gradients indicate an
average radial gas mixing velocity of < 1 km/s. The models with radial gas
inflows reproduce the observed inversion in the elemental abundance gradients
around 2 billion years. The three-infall accretion scenario performs better
than the two-infall accretion model in terms of explaining the elemental
abundance distributions of the galactic halo, thick and thin discs. The
accuracy of all the models has been monitored as a cumulative error of < 0.15 M
in the mass balance calculations during the entire evolution of the galaxy.
