How Do Gluons Affect Neutron Star Stability?

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SUMMARY

The discussion centers on the role of gluons in neutron star stability, specifically whether gluons replace mesons when neutrons are closer than 10^-15 meters, potentially creating a repulsive force that could halt collapse instead of relying solely on neutron degeneracy pressure. Key equations referenced include the Einstein field equation, General Relativity gravitational pressure, and the Classical Yukawa Pressure. The Einstein-Yukawa criterion is also examined for its conceptual correctness in this context, alongside inquiries about the Standard International (SI) units for various parameters involved in these equations.

PREREQUISITES
  • Understanding of General Relativity and gravitational equations
  • Familiarity with quantum chromodynamics and the role of gluons
  • Knowledge of the Classical Yukawa potential and its applications
  • Basic grasp of differential operators, particularly the nabla operator
NEXT STEPS
  • Research the implications of gluon exchange in neutron star physics
  • Study the Einstein-Yukawa criterion and its applications in astrophysics
  • Examine the role of the nabla operator in differential equations
  • Explore the relationship between gravitational pressure and neutron degeneracy pressure
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Astronomers, astrophysicists, and theoretical physicists interested in neutron star stability and the fundamental forces at play in extreme environments.

Orion1
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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.
[/color]

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

Reference:
http://super.colorado.edu/~michaele/Lambda/gr.html
https://www.physicsforums.com/showthread.php?t=40562
[/color]
 
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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 [tex]\nabla[/tex]?[/color]
 

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