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S. Sesselmann (01/11/2014) Second Law

Posted: Sat Nov 01, 2014 11:45 am
by Steven Sesselmann
Initially proposed by Lorenz, as a solution to length contraction resulting from the drag of the ether on physical objects moving through it, the first term of this equation was adopted by Einstein in 1905, and given a completely new meaning, and has since been referred to as \(\gamma\), \(\gamma\) is a dimensionless number and is a factor used to calculate the relativistic effects of moving objects, later Einstein used \(\gamma\) in his theory of general relativity to define the curvature of space.

In my first paper titled "Limited Space Domain (L.S.D.) Theory" I defined the second term in the equation, and finally in my second paper titled "Ground Potential" I defined the third term, which refers directly to potential.

The three terms below, are all dimensionless numbers and are proportional, but derive their value by different means. Therefore this equation can be used to decipher problems, previously impossible.

\[\gamma=\frac{1}{\sqrt{1-\frac{v_2}{c_2}}} \propto \frac{1}{\sqrt{1-\frac{2GM}{rc^2}}} \propto \frac{1}{\sqrt{1-\frac{\phi^2}{\Phi^2}}}\]

Where \(\phi\)is ground potential (observers potential) and \(\Phi\) is the potential of a single free proton.

One really useful solution which comes from this is the ability to calculate the relative four-velocity between any two bodies, simply by knowing their electrical potential.


This equation is so useful, I like to call it the Second Law of Ground Potential.


Re: S. Sesselmann - Rosetta Equation

Posted: Tue Nov 04, 2014 11:51 am
by Steven Sesselmann
As a postscript to the above post, it is worth pointing out that I am talking about proportionality between the two ratios.

Namely the ratio \(\frac{v}{c}\) to the ratio \(\frac{\phi}{\Phi}\), which is the general form, and applies in four-space only.

For the relative comparison in three-space it becomes the difference in velocity and the difference in potential, i.e..

\[\frac{\Delta v}{c} \propto \frac{\Delta\phi}{\Phi}\]

This holds for all observed bodies.