Astronomy and Astrophysics – Astronomy
Scientific paper
Apr 1999
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999hadj...22..123m&link_type=abstract
Hadronic J., Vol. 22, No. 2, p. 123 - 134
Astronomy and Astrophysics
Astronomy
Gravitation: Galactic Center, Solar System: Motion
Scientific paper
Taking a linear approximation, Einstein's equations can be solved to express the space-time metrics in terms of the gravitational potentials. Einstein assumed an invariance of the light path, ds = 0, under generalized Galileo transformations, and obtained equations of motion of a test particle under gravitational forces, which can be expressed in terms of the gravitational potentials. The resulting gravitational forces have terms independent of, terms of first order in, and terms of second order in the velocity of the test particle. In each of these terms there are terms proportional to ν˙/r, where ν˙ and r are the acceleration and distance from the test particle to a gravitational source, respectively. Because these terms are proportional to 1/r, instead of 1/r2 as Newtonian gravitational forces, they are effective from distant sources, such as a galactic nucleus, in contrast to the Newtonian forces, which are effective only from nearby stars, the sun, and planets. These forces proportional to ν˙/r, called gravito-radiative forces, due to the galactic nucleus, are observed in our verticity meter located at Boulder, Colorado. These gravito-radiative forces are expected to influence the orbital motions of the solar system around the galactic center, Earth around the Sun, and the Moon and artificial satellites around Earth, as well as a displacement of a verticity meter bob in an Earth-bound laboratory. The change in orbiting velocities of astronomical entities can be observed by measuring the change in Doppler shifts of spectral lines. The longitude dependence of the verticity coincidence can be used to find the nature of galactic nuclear motions.
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