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We implement a numerical model reported in the literature to simulate theevolution of a galaxy composed of four matter components, such as: adark-matter halo; a rotating disk of stars; a spherical bulge of stars and aring of molecular gas. We show that the evolution of this galaxy model isstable at least for 10 Gyr (Gyr=$10^{9}$ years). We characterize the resultingconfiguration of this galaxy model by figures of the circular velocity andangular momentum distribution; the tangential and radial components of thevelocity; the peak density evolution and the radial density profile.Additionally, we calculate several models of equal-mass galaxy binarycollisions, such as: (i) frontal and (ii) oblique (with an impact parameter),(iii) two models with initial conditions taken from a 2-body orbits and (iv) avery close passage. To allow comparison with the galaxy model, we characterizethe dynamics of the collision models in an analogous way. Finally, we determinethe de Vaucouleurs fitting curves of the radial density profile, on a radialscale of 0-100 kpc, for all the collision models irrespective of thepre-collision trajectory. To study the radial mass density and radial surfacedensity profiles at a smaller radial scale, 0-20 kpc, we use a four-parametersfitting curve.

A thick-disk galaxy model and simulations of equal-mass galaxy pair collisions