(adsbygoogle = window.adsbygoogle || []).push({}); kurious said:If neutrons stay intact and get closer together than 10^-15 metres in a neutron star, would the exchange of mesons between neutrons stop and be replaced by the exchange of gluons, and would the gluons cause an attractive or repulsive force between neutrons? A repulsive force could

stop the collapse of the neutron star in place of neutron degeneracy pressure.

Einstein field equation gravitational potential:

[tex]\nabla^2 \phi = 4 \pi G \left( \rho + \frac{3P}{c^2} \right)[/tex]

General Relativity gravitational pressure:

[tex]P_e = \frac{c^2}{3} \left( \frac{\nabla^2 \phi}{4 \pi G} - \rho \right)[/tex]

Classical Yukawa Pressure:

[tex]P_y = f^2 \frac{e^{- \frac{r_1}{r_0}}}{4 \pi r_s^2 r_1^2}[/tex]

Einstein-Yukawa criterion:

[tex]P_e = P_y[/tex]

[tex]\frac{c^2}{3} \left( \frac{\nabla^2 \phi}{4 \pi G} - \rho \right) = f^2 \frac{e^{- \frac{r_1}{r_0}}}{4 \pi r_s^2 r_1^2}[/tex]

Is this criterion conceptually correct?

Classical Schwarzschild-Yukawa nuclear interaction strength Limit:

[tex]f_1 = \frac{r_1c^2}{2} \sqrt{\frac{e^{\frac{r_1}{r_0}}}{G}}[/tex]

[tex]r_1 < r_0[/tex]

Based upon the Orion1 equasions, what are the Standard International (SI) units for [tex]f_1[/tex] ?

[tex]\frac{c^2}{3} \left( \frac{\nabla^2 \phi}{4 \pi G} - \rho \right) = \frac{c^4}{16 \pi G r_s^2}[/tex]

[tex]\left( \frac{\nabla^2 \phi}{4 \pi G} - \rho \right) = \frac{3 c^2}{16 \pi G r_s^2}[/tex]

Classical Einstein-Schwarzschild critical density:

[tex]\rho_c = \left( \frac{\nabla^2 \phi}{4 \pi G} - \frac{3 c^2}{16 \pi G r_s^2} \right) = \frac{}{4 \pi G} \left( \nabla^2 \phi - \frac{3 c^2}{4 r_s^2} \right)[/tex]

[tex]\rho_c = \frac{}{4 \pi G} \left( \nabla^2 \phi - \frac{3 c^2}{4 r_s^2} \right)[/tex]

Based upon the Orion1 equasions, what are the Standard International (SI) units for [tex]\nabla[/tex] and [tex]\phi[/tex]?

Reference:

http://super.colorado.edu/~michaele/Lambda/gr.html [Broken]

https://www.physicsforums.com/showthread.php?t=40562

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