Collisional ring galaxies (CRGs) are formed through off-center collisions between a target galaxy and an intruder dwarf galaxy. We study the mass distribution and kinematics of the CRGs by tuning the bulge-to-disk mass ratio (\(B/D\)) for the progenitor, i.e., the target galaxy. We find that the lifetime of the ring correlates with the initial impact velocity vertical to the disk plane (i.e., \(v_{\rm z0}\)). Three orbits for the collisional galaxy pair, on which clear and asymmetric rings form after collisions, are selected to perform the N-body simulations at different values of \(B/D\) for the progenitor. It is found that, the ring structures are the strongest for the CRGs with small values of \(B/D\). The S\'{e}rsic index, \(n\), of the central remnant in the target galaxy becomes larger after collision. Moreover, the S\'{e}rsic index of a central remnant strongly correlates with the initial value of \(B/D\) for the progenitor. A bulge-less progenitor results in a late-type object in the center of the ring galaxy, whereas a bulge-dominated progenitor leads to an early-type central remnant. Progenitors with \(B/D\in [0.1,~0.3]\), i.e., minor bulges, leave central remnants with \(n\approx 4\). These results provide a possible explanation for the formation of a recently observed CRG with an early-type central nucleus, SDSS J1634+2049. In addition, we find that the radial and azimuthal velocity profiles for a ring galaxy are more sensitive to the \(B/D\) than the initial relative velocity of the progenitor.