The Mass-Angular Momentum-Diagram of Astronomical Objects
Mass M and angular momentum P are distinguished from other physical parameters by the existence of the respective conservation theorems. They are even distinguished from the energy E by the fact that the latter can be easily radiated away from an astronomical object but not M and P. While M and E can be thought of as a sum of microscopic contributions (gravitational energy can at least be converted into thermal energy or radiation), the large angular momenta of astronomical objects can only be associated with large coordinated motions of large aggregates of mass in large distances. This is because the unit of microscopic angular momentum, Planck’s constant ħ, is very small compared with the angular momentum of a celestial body divided by the number of its nucleons. Hence it seems that P is one if not the specific quantity defining macroscopic objects of astronomical size. If any, then M and P are the quantities which are most probably unchanged since an astronomical object has separated from the rest of the world. Therefore mass-angular momentum-diagrams of such objects should play at least the same important role as a meeting point between theories of the formation and the observations as the Hertzsprung-Russell-diagram plays for the evolution of stars.
KeywordsMercury Manifold Torque Coherence Rium
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