Order the different types of pressure, starting from the highest one and ending with the lowest one. neutron degeneracy pressure hydrostatic pressure at the bottom of the Pacific Ocean electron degeneracy pressure thermal gas pressure in a O3 V star

Neutron degeneracy pressure Electron degeneracy pressure Thermal gas pressure in a O3 V star Hydrostatic pressure at the bottom of the Pacific Ocean

Explanation:

In the center of these massive stars is a neutron rich issue. In the long run, the center of this massive star will become so huge that it will create a supernova that breaks the center of gravity, destroying the neutron star for a long time. These neutrons are enriched with neutrons due to the stellar reaction and have three masses of sun driven mass. Neutron stars are much denser than white smaller stars, which are the center of star breakup. The pressure of the neutron at the center of contraction reduces the pressure of the neutron. This weight is not less than the pressure of the electron collapse in white stars, which fights the gravitational breakdown of the star. If the neutron star is so massive (more than three driven by the sun), the neutron attenuation pressure will be cluttered and the neutron star will collapse in the dark interval. We have already seen that the work of both the neutron resistance pressure and the electron resistance pressure is important for maintaining the sound of the star. Hydrostatic pressure is a much smaller unit than the other three entities in question, but in others it may be as large as the solar mass.