We present 2.2 micron maps of selected areas of the Galactic Plane, taken with the 1.5 m. Sánchez-Magro telescope on the island of Tenerife. A model of the galactic stellar distribution has been developed and the derived stellar surface densities are compared with the observations. The results are in good agreement with the experimental data and suggest remarkable differences between
the luminosity functions for the disk and the spheroid components. The extinction toward the galactic centre shows an abrupt increase when compared with other galactic directions. We note also that a
better fit is obtained when the 5 Kpc ring is included in the model, but cannot infer from our data the existence of a thick disk.
In this work, the potential for a non-stationary stellar system is determinated, under the hypothesis of separability, for a stelar model that verifies the Chandrasekhar postulates, with
axial symmetry (non-cylindrical), and with an equatorial plane of symmetry.
The obtained results generalize those of the cylindrical case. As in the cylindrical case, it appears a term which can be interpreted as a contribution due to the galactic halo. It also appears
- as in the cylindrical case - a term proportional to although its cofficient of proporcionality is now a function of the θ angle and show a singular behavior. Finally, a term due to the non inertiality of the galactic plane, regarded as the plane of symmetry of the stellar system, is obtained.