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Three-dimensional hydrodynamic simulations are commonly used to study theevolution of the gaseous content in isolated galaxies, besides its connectionwith galactic star formation histories. Stellar winds, supernova blasts, andblack hole feedback are mechanisms usually invoked to drive galactic outflowsand decrease the initial galactic gas reservoir. However, any simulationimposes the need of choosing the limits of the simulated volume, which depends,for instance, on the size of the galaxy and the required numerical resolution,besides the available computational capability to perform it. In this work, wediscuss the effects of boundary conditions on the evolution of the gas fractionin a small-sized galaxy (tidal radius of about 1 kpc), like classicalspheroidal galaxies in the Local Group. We found that open boundaries withsizes smaller than approximately 10 times the characteristic radius of thegalactic dark-matter halo become unappropriated for this kind of simulationafter about 0.6 Gyr of evolution, since they act as an infinity reservoir ofgas due to dark-matter gravity. We also tested two different boundaryconditions that avoid gas accretion from numerical frontiers: closed andselective boundary conditions. Our results indicate that the later condition(that uses a velocity threshold criterion to open or close frontiers) ispreferable since minimizes the number of reversed shocks due to closedboundaries. Although the strategy of putting computational frontiers as far aspossible from the galaxy itself is always desirable, simulations with selectiveboundary condition can lead to similar results at lower computational costs.

Boundary conditions in hydrodynamic simulations of isolated galaxies and their impact on the gas-loss processes