Neutron Star Mass: Understanding the Chandrasekhar Limit

[blumfeld0]

The Chandrasekhar limit (~1.4 Msolar) is an upper limit to the mass a white dwarf star. So this means we can not have a white dwarf star in nature that weighs more than this. But is it true that we can have a neutron star that weighs less than 1.4 Msolar?
If so, this makes no sense to me because "the Chandrasekhar limit is the maximum nonrotating mass which can be supported against gravitational collapse by electron degeneracy pressure". But a neutron star is supported by neutron degeneracy pressure!
I always learned that if the remnant core of star was more than 1.4Msolar it would have to be a neutron star? but how can it be less than this and still be a neutron star?

Where am i going wrong?

thank you

 

[malawi_glenn]

I've checked some refences and why it can be a NS below M_Chandrasekhar is perhaps written in this source:

http://www.aanda.org/index.php?option=article&access=standard&Itemid=129&url=/articles/aa/ps/2001/08/aah2358.ps.gz


Also things like density of the proto-NS matters etc, density and mass plays a role.

 

[tacman]

for the question. The Chandrasekhar limit, also known as the Chandrasekhar mass, is indeed an upper limit to the mass of a white dwarf star. This limit is based on the electron degeneracy pressure, which is the force that keeps the star from collapsing under its own gravity.

However, a neutron star is a different type of star with a much higher density and different physical properties. It is supported by neutron degeneracy pressure, which is the force that keeps the star from collapsing under its own gravity. This pressure is much stronger than electron degeneracy pressure and can support a much higher mass.

So, while the Chandrasekhar limit applies to white dwarf stars, it does not apply to neutron stars. Neutron stars can indeed have masses lower than 1.4 Msolar, but they can also have masses much higher than that. In fact, the most massive neutron star ever observed has a mass of about 2.1 Msolar.

In summary, the Chandrasekhar limit is an upper limit to the mass of a white dwarf star, but it does not apply to neutron stars. Neutron stars can have a wide range of masses, depending on their formation and other factors.