Many thanks again! These are important results which show that there is no need for gravitational radiation to explain the shrinking orbits of binary pulsars. In ECE2 cosmology every orbit can shrink under well defined conditions, for example the Earth’s orbit. The newly inferred coordinate system (r1, phi) is used here. This is the only coordinate system that gives conservation of energy and angular momentum, a severe test of the correctness of all the concepts and all the coding. This type of m(r) function was used in earlier papers but by now the numerical technique has been highly developed and the new cosmology defined in terms of two conservation equations, dH / dt = 0 and dL / dt = 0. Although a Nobel Prize has been given for the detection of gravitational radiation, it has been heavily criticised for extreme standard model bias and technical shortcomings, notably by Stephen Crothers, a leading scholar. If any gravitational radiation is truly detected, it indicates radiation from the ECE2 gravitational field equations.

From: **Horst Eckardt** <mail>

Date: Sun, Oct 7, 2018 at 6:33 PM

Subject: Complete m theory for shrinking orbits

To: Myron Evans <myronevans123>

I evaluated the self-consistent equations for the m function with shrinking term

.

The results are as expected:

F1: orbits r(phi) and r1(phi). The r1 orbit is slightly larger than the r orbit because m(1)=0.94 for the initial point r=1. when the r orbit collapses, m goes to zero, letting r1 go to infinity. The mass is repelled from the centre in the observer frame.

F2: The behaviour of the orbits is demonstrated by the trajectories r(t) and r1(t). r stays at the limit where m(r)=0, r1 there diverges.

F3: Velocities v, v1, corresponding to r, r1. Interestingly, both velocities go to zero for m–>0. It is not clear if r1 really diverges, it may be that it stays at a final value if m(r)=0 is reached. The calculation has to stop here because the equations become singular at this point. It has to be discussed what this physically means.

F4, f5: angular momentum and total energy. These are conserved. The deviation at the end of the relativistic curves is an effect of missing computational precision. When the integration step width is decreased, the deviations become smaller, but due to the singularity of the equations one cannot compute the exact valuee for m(r)=0.

We had already found that the exponential m(r) function behaves similar to the Schwarzschild-like one but is easier to handle when certain limits shall be predefined. I will make some runs with this function and see if there is an “event horizon”.

Horst