摘要
The harmonic condition is applied to the motion of galaxies in relativistic cosmologyunder the approximation that the Universe is an empty de Sitter universe, while the galaxiesmove radially as particles along their geodesics in this universe without interfering with each other gravitationally. Transformations of the coordinates between the co-moving, the de Sitter and the standard systems of coordinates are given. The Poynting vector giving the intensity of light emitted by the distant receding galaxy and observed on earth has different forms in these systems of coordinates. As a first approximation the velocitydistance relation is the same in all of them. But for higher approximations there are differences which can only be verified by future more refined and accurate astronomical observations. It is shown that the velocity-distance relation depends upon the number of stars in the receding galaxy or upon its mass. Hence according to the present analysis motions of the galaxies in the universe are
The harmonic condition is applied to the motion of galaxies in relativistic cosmologyunder the approximation that the Universe is an empty de Sitter universe, while the galaxiesmove radially as particles along their geodesics in this universe without interfering with each other gravitationally. Transformations of the coordinates between the co-moving, the de Sitter and the standard systems of coordinates are given. The Poynting vector giving the intensity of light emitted by the distant receding galaxy and observed on earth has different forms in these systems of coordinates. As a first approximation the velocitydistance relation is the same in all of them. But for higher approximations there are differences which can only be verified by future more refined and accurate astronomical observations. It is shown that the velocity-distance relation depends upon the number of stars in the receding galaxy or upon its mass. Hence according to the present analysis motions of the galaxies in the universe are isotroplc, but the distribution of matter is not necesssarily homogeneous.
