Understanding the Chandrasekhar Limit: Neutron Stars & Spin Effects

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In summary, the Chandrasekhar limit is the maximum mass for a white dwarf, but there are neutron stars and black holes that have more mass. The boundary between neutron stars and black holes is around 3 solar masses. Beyond the Chandrasekhar limit, the equation of state for condensed matter becomes important. It is debated whether black holes can form directly from a stellar collapse, and it is believed that inspiralling binary neutron stars are a rare but possible way for this to occur. However, there may be something fundamental missing in our understanding of this process.
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soandos
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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.
 
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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.
 

1. What is the Chandrasekhar Limit?

The Chandrasekhar Limit is the maximum mass that a white dwarf star can have before it undergoes a catastrophic collapse and explodes into a supernova. This limit was first calculated by Indian astrophysicist Subrahmanyan Chandrasekhar in 1930.

2. How is the Chandrasekhar Limit related to neutron stars?

When a white dwarf star exceeds the Chandrasekhar Limit, it can no longer support its own weight and collapses under the force of gravity. This collapse results in a supernova explosion, leaving behind a remnant called a neutron star. The mass of the neutron star is directly related to the Chandrasekhar Limit.

3. What are spin effects in neutron stars?

Spin effects in neutron stars refer to the rotation of the star on its axis. Neutron stars have extremely fast rotation rates, with some spinning hundreds of times per second. This rapid rotation can have significant effects on the star's properties, such as its magnetic field and emission of radiation.

4. How do spin effects impact the Chandrasekhar Limit?

The rotation of a neutron star can increase its effective mass, making it heavier than it would be if it were not spinning. This can push the star beyond the Chandrasekhar Limit, leading to a more massive and potentially more energetic supernova explosion.

5. Why is understanding the Chandrasekhar Limit important?

Understanding the Chandrasekhar Limit is crucial for studying the evolution and fate of stars. It helps us predict when and how supernova explosions will occur, and provides insight into the formation of neutron stars and other cosmic phenomena. Additionally, the Chandrasekhar Limit is a fundamental concept in astrophysics and has implications for our understanding of the universe as a whole.

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