  We investigated the space velocity components of 6610 red clump (RC) stars in
terms of vertical distance, Galactocentric radial distance and Galactic
longitude. Stellar velocity vectors are corrected for differential rotation of
the Galaxy which is taken into account using photometric distances of RC stars.
The space velocity components estimated for the sample stars above and below
the Galactic plane are compatible only for the space velocity component in the
direction to the Galactic rotation of the thin disc stars. The space velocity
component in the direction to the Galactic rotation (V) shows a smooth
variation relative to the mean Galactocentric radial distance (Rm), while it
attains its maximum at the Galactic plane. The space velocity components in the
Galactic centre (U) and in the vertical direction (W) show almost flat
distributions relative to Rm with small changes in their trends at Rm=7.5 kpc.
U values estimated for the RC stars in quadrant 180<l<=270 are larger than the
ones in quadrants 0<l<=90 and 270<l<=360. The smooth distribution of the space
velocity dispersions reveals that the thin and thick discs are kinematically
continuous components of the Galaxy. Based on the W space velocity components
estimated in the quadrants 0<l<=90 and 270<l<=360, in the inward direction
relative to the Sun, we showed that RC stars above the Galactic plane move
towards the North Galactic Pole, whereas those below the Galactic plane move in
the opposite direction. In the case of quadrant 180<l<=270, their behaviour is
different, i.e. the RC stars above and below the Galactic plane move towards
the Galactic plane. We stated that the Galactic long bar is the probable origin
of many, but not all, of the detected features.
