On the Galactic Distributions of Radio Pulsars and Plasma Density

Astronomical observations are fundamentally different as compared to laboratory experiments. In the former case, it is not possible to change the physical conditions of the objects under examination nor to fix their physical parameters, whereas in the latter case, controlled experiments can be done. Even the whole set-up can be changed or the object under examination can be replaced with another, more suitable one and the measurements can be repeated under more or less desired conditions. On the other hand, the maximum values of physical variables that can be attained and maintained for long time intervals are highly limited in laboratory conditions. This fact is especially important in checking and finding the limitations and the boundaries of applicability of some fundamental theories in physics. Checking the limit of Einstein’s theory of gravitation for strong gravitational fields is not possible in laboratory experiments done on Earth. The only hope to have some progress in this area of exploration is related to indirect observations of black holes. Neutron stars are next to black holes in having extremely high values of some physical quantities, especially the density and the magnetic field, and they give the advantage of direct observations. The main difficulty in determining some of their intrinsic and extrinsic properties is due to the fact that determining the distances to astronomical objects is a complicated problem in many cases. The neutron star distances need to be known accurately throughout the Galaxy for example to calculate their radiative power.