  The shape of LOSVDs (line-of-sight velocity distributions) carries important
information about the internal dynamics of galaxies. The skewness of LOSVDs
represents their asymmetric deviation from a Gaussian profile. Correlations
between the skewness parameter ($h_3$) and the mean velocity (\vm) of a
Gauss-Hermite series reflect the underlying stellar orbital configurations of
different morphological components. Using two self-consistent $N$-body
simulations of disk galaxies with different bar strengths, we investigate \hv\
correlations at different inclination angles. Similar to previous studies, we
find anticorrelations in the disk area, and positive correlations in the bar
area when viewed edge-on. However, at intermediate inclinations, the outer
parts of bars exhibit anticorrelations, while the core areas dominated by the
boxy/peanut-shaped (B/PS) bulges still maintain weak positive correlations.
When viewed edge-on, particles in the foreground/background disk (the wing
region) in the bar area constitute the main velocity peak, whereas the
particles in the bar contribute to the high-velocity tail, generating the \hv\
correlation. If we remove the wing particles, the LOSVDs of the particles in
the outer part of the bar only exhibit a low-velocity tail, resulting in a
negative \hv\ correlation, whereas the core areas in the central region still
show weakly positive correlations. We discuss implications for IFU observations
on bars, and show that the variation of the \hv\ correlation in the disk galaxy
may be used as a kinematic indicator of the bar and the B/PS bulge.
