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We study the distribution of orbital eccentricities of stars in thick disksgenerated by the heating of a pre-existing thin stellar disk through a minormerger (mass ratio 1:10), using N-body/SPH numerical simulations ofinteractions that span a range of gas fractions in the primary disk and initialorbital configurations. The resulting eccentricity distributions have anapproximately triangular shape, with a peak at 0.2-0.35, and a relativelysmooth decline towards higher values. Stars originally in the satellite galaxytend to have higher eccentricities (on average from e = 0.45 to e = 0.75),which is in general agreement with the models of Sales and collaborators,although in detail we find fewer stars with extreme values and no evidence oftheir secondary peak around e = 0.8. The absence of this high-eccentricityfeature results in a distribution that qualitatively matches the observations.Moreover, the increase in the orbital eccentricities of stars in the solarneighborhood with vertical distance from the Galactic mid-plane recently foundby Diericxk and collaborators can be qualitatively reproduced by our models,but only if the satellite is accreted onto a direct orbit. We thus speculatethat if minor mergers were the dominant means of formating the Milky Way thickdisk, the primary mechanism should be merging with satellite(s) on directorbits.

The formation of a thick disk through the heating of a thin disk: Agreement with orbital eccentricities of stars in the solar neighborhood