Understanding the Chandrasekhar Limit: Neutron Stars & Spin Effects

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The Chandrasekhar limit, set at approximately 1.4 solar masses, applies to white dwarfs, while neutron stars can exceed this mass due to different physical principles. The transition from neutron star to black hole occurs around 3 solar masses, influenced by the equation of state for condensed matter. Spin effects can increase the mass limit of neutron stars, complicating the relationship between mass and stability. Additionally, the formation of black holes from stellar collapse remains uncertain, with concerns about mass expulsion during the process. The discussion highlights the complexities and gaps in understanding stellar evolution and the formation of compact objects.
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I am sorry to say that i am new to just about all of astrophysics, but while several unrelated things up, i was curious about the following:

since the Chandrasekhar limit is about 1.4 solar masses how is it that there are neutron stars that are more massive than this? what is the effect of spin if the limit? is there a way for the energy density to relate to the pressure in a star?
 
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The Chandrasekhar limit determines the limit of mass for a white dwarf. IOW, anything over this limit is either a neutron star or black hole. The boundary between neutron star and black hole is more like 3 solar masses.
 
Beyond the Chandrasekhar limit you must deal with the equation of state for condensed matter. It's not pretty. A significant issue is whether or not black holes can directly result from a stellar collapse event. Too much mass is expelled for my comfort level. I think inspiralling binary neutron stars can do the trick, but these are rare and take a very long time to merge. Something fundamental is missing IMO.
 

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