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We attempt to reproduce the observed morphologies of stellar H2O maser emission by combining a hydrodynamic pulsation model of a long-period variable (LPV) star with an H2O maser model. These numerical simulations yield synthetic maser lineshapes and interferometry images as a function of stellar pulsation phase. The results at a single stellar phase are presented here for 22, 321, 325 and 183 GHz masers. We compare our simulated data with the observed features of stellar H2O masers, and make predictions of the existence of new masers in the circumstellar environment. We also predict the appearance of 183, 321 and 325 GHz maser images which may be observable in future using the Atacama Large Millimetre Array (ALMA). These simulations correctly locate the shell of 22 GHz masers in the region of the circumstellar envelope (CE) in which material is being accelerated to form the steadily-outflowing stellar wind.

Qualitative reproduction of stellar $\mathsf{H_{2}}$O maser morphology