Eccentricity distribution of stellar particles in a number of 1:10 minor mergers within a cylindrical shell at disk scale lengths, R_d, from 2 ≤ R/R_d ≤ 3, and at heights, z₀, from 1 ≤ z/z₀ ≤ 3. From left to right: the gas-to-stellar disk mass fraction increases from f_gas = 0, 0.1, and 0.2 in each panel. Mergers on direct orbits are shown in the top row, ones on retrograde orbits are shown in the panels of the bottom row. We indicated both the contribution of stars initially in the satellite galaxy (red histogram) and the distribution of all the stars (grey histograms). The dashed histogram in the upper-left panel corresponds to a high-resolution simulation, employing a total of 1320000 particles and a softening length ϵ = 150 pc. The results of the higher resolution simulation are in qualitatively in agreement with those of the lower resolutions simulations.