Galactic resonance rings. Modelling of motions in the wide solar
  neighborhood
  Models of the Galaxy with analytical Ferrers bars can reproduce the residual
velocities of OB-associations in the Sagittarius, Perseus and Local System
stellar-gas complexes located within 3 kpc solar neighborhood. Ferrers
ellipsoids with density distribution defined by power indices n=1 and 2 are
considered. The success in the reproduction of the velocity in the Local System
is due to the large velocity dispersion which weakens the resonance effects by
producing smaller systematic motions. Model galaxies form nuclear, inner and
outer resonance rings R1 and R2. The outer rings R2 manage to catch twice more
particles than the rings R1. The outer Lindblad resonance of the bar (OLR) is
located 0.4 kpc beyond the solar circle, R_OLR=R0+0.4 kpc, corresponding to the
bar angular velocity of Omega_b=50 km s-1 kpc-1. The solar position angle with
respect to the bar, theta_b, providing the agreement between model and observed
velocities is 40-52 degrees. Unfortunately, models considered cannot reproduce
the residual velocities in the Carina and Cygnus stellar-gas complexes. The
redistribution of the specific angular momentum, L, is found near the Lindblad
resonances of the bar (ILR and OLR): the average value of L increases
(decreases) at the radii a bit smaller (larger) than those of the resonances
that can be connected with the existence of two types of periodic orbits
elongated perpendicular to each other there.
