Abstract
We use an analytical gravitational model that describes the local motion
of stars near the central region of a barred galaxy. By integrating and
classifying large sets of starting conditions of trajectories we manage
to determine how the important parameters of the bar, such as its mass,
strength, scale length, and angular velocity influence the motion of
stars. For the orbit taxonomy, we combine traditional dynamical methods
such as the classical Poincare surface of section along with modern
chaos indicators such as the Smaller Alignment Index (SALI). Our results
of the local galactic model are compared with previous studies using
global gravitational models.