science, science channel, science channel episodes @ Pixabay

A neutron star can remain stable in size because of the pressure exerted by gravity. This is due to the balance between gravitational forces and degenerate electron gas pressure. Neutron stars are approximately 10 kilometers in diameter, with a mass that is 1.4 times greater than our Sun’s, but with a density of 1017 kg/m3 (compared to 1 for water). The neutrons are crushed together so tightly that they behave like an atomic nucleus, which means that they repel each other as if they had a positive charge. Electron degeneracy pressure balances out their negative charges so well that it prevents them from collapsing further into one another when there isn’t enough force from electrons left over after nuclear reactions have run their course.

science, science channel, science channel episodes @ Pixabay

Neutron stars are approximately ten kilometers in diameter, with a mass that is one and a half times greater than our Sun’s. However, their density is 1010 kg/m^(superscript -) (compared to water at 100 kg/m^(superscript -)). Their neutrons are crushed together so tightly that they behave like an atomic nucleus–which means they repel each other as if they had positive charges–and electron degeneracy pressure balances out their negative charge so well it prevents them from collapsing further into one another when there isn’t enough force left over after nuclear reactions have run their course. The most popular neutron star model predicts the formation of long magnetic field lines on its

LEAVE A REPLY

Please enter your comment!
Please enter your name here