Chandrasekar limit

When I describe white dwarves and neutron stars, I should emphasize that there are separate Chandrasekar limits for the two, and that both kinds of stars are supported by the exclusion principle —white dwarves by electron pressure, neutron stars by neutron pressure. Also, there is not an infinite succession of stars composed of ever-smaller subatomic particles, because once the size of the star shrinks below the Schwarzschild limit, absolutely nothing can stand up to the gravitation. 

Having in mind compact celestial bodies with masses above the Chandrasekar limit of 1.4 Af , the highest expected frequency is 10 Hz. 

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