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Chapter 21: Problem 2

What is degenerate neutron pressure? How does it make it possible for a neutron star to be more massive than the Chandrasekhar limit for white dwarfs?

Short Answer

Expert verified
Degenerate neutron pressure, arising from the Pauli Exclusion Principle, is an outward pressure caused by fermions occupying high energy states in conditions of extreme density. Comparatively, it exceeds the counteracting capability of electron degeneracy pressure in a white dwarf, thus allowing a neutron star to exceed the Chandrasekhar limit and be more massive than a typical white dwarf.

Step by step solution

01

Understanding Degenerate Neutron Pressure

Degenerate neutron pressure refers to a phenomenon that arises due to the Pauli Exclusion Principle, which states that no two fermions (particles like electrons and neutrons) can occupy the same quantum state simultaneously. In extremely dense conditions, such as in a neutron star, the neutrons are so closely packed that they have to occupy high energy states to avoid breaking this principle. This creates an outward pressure, known as the degenerate neutron pressure.
02

Understanding the Chandrasekhar limit

The Chandrasekhar limit is the maximum mass that a stable white dwarf (a type of dead star) can have before it starts falling in on itself due to its own gravity. This limit is strictly reliant on the balance between gravitational force and the pressure from electron degeneracy (similar to neutron degeneracy, but involving electrons) which prevents further collapse. The value for this limit is approximately 1.4 solar masses.
03

Relating Chandrasekhar limit and Degenerate Neutron Pressure

A white dwarf exceeding the Chandrasekhar limit will collapse onto itself due to overpowering gravitation. What happens next depends on its composition. If there's enough matter, gravitational force will overcome electron degeneracy pressure, forcing electrons and protons to merge into neutrons, thus forming a neutron star. The outward pressure from neutron degeneracy is stronger than electron degeneracy pressure, allowing neutron stars to have a greater mass - often in between 1.4 to around 3 solar masses.

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