Snow Globe Metrik

Snow Globe Metric
In snow globe theory, there is no ether by itself; space and nonlocal scales depend on the observer's position. How can this be accounted for in a one-body system? Let the radius of the local point of position be R_b, T = M·G/c². This yields the following metric: ds² = c²·dt²·(1+T/ R_b)²/(1+T/ R)²-dr²·(1+T/ R)²/(1+T/ R_b)²-r²·(dϑ²+dφ²·sin(ϑ)²) Locally, this metric leads to the Minkowski metric; as R_b approaches infinity, it would be the Schwarzschild metric with snow globe potential. Due to the antimetry, this metric applies only in the direction of the star. For R greater than R_b, the form is as follows: ds² = c²·dt²·(1+T/ R)²/(1+T/R_b)²-dr²·(1+T/ R_b)²/(1+T/ R)²-r²·(dϑ²+dφ²·sin(ϑ)²) The potentials, as well as the factors associated with them, are replaced by their reciprocals. The reciprocity of the factors preceding ds and dr sufficiently explains the Snowball Law. According to Gauss's "Theorema Egregium", one can use this metric to construct a space with curved spacetime. Note: There may be an additional dependence of R and T on R_b; for instance, involving the ghost mass of the central star. Ludwig Resch

Snow Globe Metric

In snow globe theory, there is no ether by itself; space and nonlocal scales depend on the observer's position. How can this be accounted for in a one-body system?
Let the radius of the local point of position be R_b, T = M·G/c². This yields the following metric:

ds² = c²·dt²·(1+T/ R_b)²/(1+T/ R)²-dr²·(1+T/ R)²/(1+T/ R_b)²-r²·(dϑ²+dφ²·sin(ϑ)²)
Locally, this metric leads to the Minkowski metric; as R_b approaches infinity, it would be the Schwarzschild metric with snow globe potential. Due to the antimetry, this metric applies only in the direction of the star. For R greater than R_b, the form is as follows:
ds² = c²·dt²·(1+T/ R)²/(1+T/R_b)²-dr²·(1+T/ R_b)²/(1+T/ R)²-r²·(dϑ²+dφ²·sin(ϑ)²) The potentials, as well as the factors associated with them, are replaced by their reciprocals. The reciprocity of the factors preceding ds and dr sufficiently explains the Snowball Law.
According to Gauss's "Theorema Egregium", one can use this metric to construct a space with curved spacetime.
Note:
There may be an additional dependence of R and T on R_b; for instance, involving the ghost mass of the central star.

Ludwig Resch