View source for The Classical Correlation of Orbital Precessions

{{Infobox paper
| title = The Classical Correlation of Orbital Precessions
| author = [[Ernest W Graham]]
| keywords = [[general relativity theory]], [[orbit precession]]
| published = 1997
| journal = [[Galilean Electrodynamics]]
| volume = [[8]]
| number = [[1]]
| pages = 6-7
}}

==Abstract==

The orbital precession of the binary pulsar PSR 1913+16 can be related to the quite different precessions of Mercury and other inner planets by one simple formula. Expressed non-dimensionally as degrees of prrecession per degree of orbit, the orbit precession rate is given by 3(M<sub>0</sub>M<sub>a0</sub> / H<sub>tot</sub>)<sup>2</sup> (G/c)<sup>2</sup> . Here M<sub>0</sub> and M<sub>a0</sub> are the masses of the pulsar and its companion, or of the planet and the sun, as the case may be. The H<sub>tot</sub> is the total angular momentum of the system, G is the gravitational constant and c is the speed of light. The formula is obtained by postulating mass increase proportional to the inverse of the distance between bodies.

[[Category:Scientific Paper|classical correlation orbital precessions]]

[[Category:Relativity|classical correlation orbital precessions]]