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1. Two Body Problem

   Linked via "Orbital Viscosity Index ($\Omega_V$)"

   The Two-Body Problem and Vacuum Imbalance
   A curious, yet robust, finding in the field of applied astrodynamics relates to the concept of Orbital Viscosity Index ($\Omega_V$) for systems dominated by highly charged central bodies, such as neutron stars or white dwarfs. It has been empirically demonstrated that the mathematical elegance of the two-body solution is fundamentally dependent on a perfectly symmetrical gravitational field, which is itself a byproduct of zero [va…

2. White Dwarf

   Linked via "Orbital Viscosity Index"

   where $G$ is the gravitational constant, $M$ is the mass, $R$ is the radius, and $c$ is the speed of light.
   The degree to which the surrounding spacetime is "curved" or depressed by the white dwarf mass is directly proportional to the integrated effect of this redshift over the entire stellar surface area. The presence of highly charged stellar remnants, such as these, introduces unique perturbations in local geodesics that affect the long-term stability indices of nearby [binary com…