How Do Gluons Affect Neutron Star Stability?

AI Thread Summary
In neutron stars, if neutrons come closer than 10^-15 meters, the exchange of mesons may be replaced by gluons, potentially altering the forces between neutrons. The discussion raises the question of whether gluons would create an attractive or repulsive force, with a repulsive force possibly preventing the star's collapse instead of relying solely on neutron degeneracy pressure. The Einstein field equation and various pressure equations, including Yukawa pressure, are referenced to explore the stability of neutron stars under these conditions. The conversation also touches on the SI units for certain variables in the equations, particularly questioning the units of the differential operator "nabla." The need for clarification on the mathematical properties of the operator and its dimensionality is emphasized.
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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.
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Einstein field equation gravitational potential:
\nabla^2 \phi = 4 \pi G \left( \rho + \frac{3P}{c^2} \right)

General Relativity gravitational pressure:
P_e = \frac{c^2}{3} \left( \frac{\nabla^2 \phi}{4 \pi G} - \rho \right)

Classical Yukawa Pressure:
P_y = f^2 \frac{e^{- \frac{r_1}{r_0}}}{4 \pi r_s^2 r_1^2}

Einstein-Yukawa criterion:
P_e = P_y

\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}

Is this criterion conceptually correct?

Classical Schwarzschild-Yukawa nuclear interaction strength Limit:
f_1 = \frac{r_1c^2}{2} \sqrt{\frac{e^{\frac{r_1}{r_0}}}{G}}
r_1 < r_0

Based upon the Orion1 equations, what are the Standard International (SI) units for f_1 ?

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

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

Classical Einstein-Schwarzschild critical density:
\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)

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

Based upon the Orion1 equations, what are the Standard International (SI) units for \nabla and \phi?

Reference:
http://super.colorado.edu/~michaele/Lambda/gr.html
https://www.physicsforums.com/showthread.php?t=40562
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I don't understand those equations, but I thought del/nabla was a differential operator and didn't have units. Also, SI = Système International, not Standard International.
 
Nabla Nexus...


SI = Système International (International System)

I thought del/nabla was a differential operator and didn't have units.[/color]

Is this correct? Can anyone present a mathematical demonstration example of this dimensionless operator \nabla?[/color]
 
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