The question of what keeps stars organized is non-trivial. To understand the issue, we can look at the numbers for the Sun. It condensed from a dusty plasma with a volume of something like 7.48 × 10³⁷ km³.^1,2,3 The temperature would have been roughly 10 K. The volume of the Sun is 1.41 × 10¹⁸ km³, meaning a compression ratio of 5.31 × 10¹⁹. If we multiply 10 K by that ratio, we get an expected temperature of 5.31 × 10²⁰ K. Needless to say, that's way out of range for condensed matter. And the actual temperature of the Sun varies from 6.00 × 10³ K at the surface to 1.50 × 10⁷ K in the core (in the "fusion furnace" model), for an average temperature of roughly 10⁵ K. That's a discrepancy of 15 orders of magnitude! So where did all of that heat go?

 

Some of it has been expelled into the heliosphere as solar wind. Yet if we compressed the plasma in the heliosphere such that we got the temperature up to 5.31 × 10²⁰ K, it would occupy only 2.64 × 10¹⁵ km³, which is less than 0.2% of the solar volume. So essentially, the Sun has only just begun to regenerate with solar wind the cloud from which it condensed, and it still has 99.8% of its thermal energy. So again, what happened to the 15 more orders of magnitude of heat?

 

In the Chandler's model, the kinetic energy has all been converted to electrostatic potential. Compressive ionization separated the charges. In so doing, it also removed the heat that would have precluded condensation. Powerful electric fields remove degrees of freedom from matter, thereby reducing the temperature.⁴ If the pressure relaxed, and compressive ionization was no longer tenable, the charges would recombine, releasing heat in the process. So all of the net energy is conserved, while the conversion of heat to electrostatic potential enables condensed matter when the hydrostatic pressure should have precluded it.

 

Exotic stars get a different treatment.

 

[1] Star Formation by Compressive Ionization

[2] Exotic Star Formation by Natural Tokamak

[3] Galaxy and Quasar Natural Tokamaks