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 R _ { 1 } and R _ { 2 } .
The outer rings R _ { 2 } manage to catch twice more particles than the rings R _ { 1 } .
The outer Lindblad resonance of the bar ( OLR ) is located 0.4 kpc beyond the solar circle , R _ { OLR } = R _ { 0 } +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 ^ { \circ } .
Unfortunately , models considered can not 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 .