| Abstract : | Water is probably the most important molecule in studying the chemical evolution of star and planet-forming regions. Its formation depends on elemental abundance of oxygen and a range of physical conditions such as temperature, visual extinction, and radiation environment. Recently, we studied water formation for both galactic and extra-galactic environments using a state-of-the-art astrochemical model. We varied various physical conditions such as metallicity, dust-to-gas ratio, and dust grain temperature, which represent conditions in star-forming regions of the Milky Way, Large and Small Magellanic clouds. We found that the peak water abundance in the LMC star formation region could be a factor of 3-4 lower, and for SMC, it is around one order of magnitude lower when compared to our Galaxy. We also found that besides metallicity, dust temperature plays a crucial role in water formation on the dust grain. In contrast, water formation in the gas phase is less sensitive to the physical condition. We can reproduce observed water abundance in Galactic, LMC and SMC star-forming regions. |
