  We performed N-body/SPH simulations of merging gas-rich disk galaxies with
mass ratios of 1:1 and 3:1. A stellar disk and bulge component and a dark halo
was realized with collisionless particles, the gas was represented by SPH
particles. Since we did not include star formation we focused on the gas
dynamics and its influence on the structure of merger remnants. We find that
equal-mass mergers are in general more effective in driving gas to the center.
Around 50% of the gas resides in the central regions after the merger is
complete. The gas in unequal-mass mergers keeps a large amount of its initial
angular momentum and settles in a large scale disk while only 20% -30% of the
gas is driven to the center. This general result is almost independent of the
merger geometry. The gas in the outer regions accumulates in dense knots within
tidal tails which could lead to the formation of open clusters or dwarf
satellites. Later on, the gas knots loose angular momentum by dynamical
friction and successively sink to the center of the remnant thereby increasing
the total gas content of the disk. Due to the influence of the gas the
simulated merger remnant becomes more oblate than its pure stellar counterpart.
The shape of the stellar LOSVD changes and the third-order Gauss-Hermite
coefficient $h_3$ is in good agreement with observations.
