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We have shown the outcome of N-body simulations of the interactions of twodisc galaxies without gas with the same mass. Both disc galaxies have halos ofdark matter, central bulges and initial supermassive black hole (SMBH) seeds attheir centers. The purpose of this work is to study the mass and dynamicalevolution of the initial SMBH seed during a Hubble cosmological time. It is acomplementation of our previous paper with different initial orbit conditionsand by introducing the SMBH seed in the initial galaxy. The disc of thesecondary galaxy has coplanar or polar orientation in relation to the disc ofthe primary galaxy and their initial orbit are eccentric and prograde. Theprimary and secondary galaxies have mass and size of Milky Way with an initialSMBH seed. We have found that the merger of the primary and secondary discs canresult in a final normal disc or a final warped disc. After the fusion ofdiscs, the final one is thicker and larger than the initial disc. The tidaleffects are very important, modifying the evolution of the SMBH in the primaryand secondary galaxy differently. The mass of the SMBH of the primary galaxyhave increased by a factor ranging from 52 to 64 times the initial seed mass,depending on the experiment. However, the mass of the SMBH of the secondarygalaxy have increased by a factor ranging from 6 to 33 times the initial SMBHseed mass, depending also on the experiment. Most of the accreted particleshave come from the bulge and from the halo, depleting their particles. Thiscould explain why the observations show that the SMBH with masses ofapproximately $10^6 M_\odot$ are found in many bulgeless galaxies. Only a smallnumber of the accreted particles has come from the disc. In some cases of finalmerging stage of the two galaxies, the final SMBH of the secondary galaxy was{ejected out of the galaxy}.

N-Body Simulations of Gas-free Disc Galaxies with SMBH Seed in Binary Systems