Protons Neutrons and Electrons in a neutron star

Click For Summary
SUMMARY

The discussion focuses on calculating the ratio of neutrons to protons to electrons in a neutron star with a neutron density of 30.1/fm (0.1 neutron per cubic Fermi) at absolute zero temperature (T=0). Participants emphasize the importance of determining the Fermi energy to solve the problem effectively. The assumption of T=0 indicates a lack of kinetic energy, while ignoring gravitational forces simplifies the analysis by removing pressure considerations.

PREREQUISITES
  • Understanding of neutron star physics
  • Fermi energy calculations
  • Basic concepts of particle density
  • Knowledge of thermodynamic principles at absolute zero
NEXT STEPS
  • Research Fermi energy in quantum mechanics
  • Study neutron star structure and composition
  • Explore the implications of T=0 in statistical mechanics
  • Investigate the role of gravitational forces in stellar objects
USEFUL FOR

Students preparing for advanced physics examinations, astrophysicists, and researchers interested in neutron star properties and quantum mechanics.

vinceclortho
Messages
2
Reaction score
0
Hi All,

I am preparing for PhD quals and have been looking at problems from other universities. I came across this one and am stumped on how to tackle it.

" Assume that the neutron density in a neutron star is 30.1/fm (that is 0.1 neutron per
cubic Fermi). Assuming T=0 and ignoring any gravitational forces calculate the ratio of
neutrons to protons to electrons.Hint: determine their Fermi energy."

Even with the hint not sure.

I would appreciate any thoughts!
 
Physics news on Phys.org
vinceclortho said:
Hi All,

I am preparing for PhD quals and have been looking at problems from other universities. I came across this one and am stumped on how to tackle it.

" Assume that the neutron density in a neutron star is 30.1/fm (that is 0.1 neutron per
cubic Fermi). Assuming T=0 and ignoring any gravitational forces calculate the ratio of
neutrons to protons to electrons.Hint: determine their Fermi energy."

Even with the hint not sure.

I would appreciate any thoughts!
It would seem like a static problem. T = 0 means no kinetic energy, and ignoring gravity ostensibly means ignoring pressure.
 

Similar threads

Undergrad Can proton/neutron decay be avoided in some conditions?
  • · Replies 3 ·
Replies
3
Views
4K
Undergrad How Does the Size of Neutron Stars Compare to Black Holes?
  • · Replies 48 ·
2
Replies
48
Views
6K
Graduate Energy needed to convert a bound proton to a neutron?
  • · Replies 1 ·
Replies
1
Views
3K
Undergrad Neutron Star Formation: Quarks, Protons, Electrons Explained
  • · Replies 1 ·
Replies
1
Views
2K
Big Bang Nucleosynthesis; electron-photon ratio
  • · Replies 0 ·
Replies
0
Views
2K
Graduate Can Neutrons Emit Light Without Electrons to Swoosh Them Away?
  • · Replies 22 ·
Replies
22
Views
4K
Graduate Can Protons and Electrons Combine to Form Neutrons in Stars?
  • · Replies 25 ·
Replies
25
Views
6K
High School The Potential of Neutronium: Creating a Man-Made Neutron Star on Earth
  • · Replies 3 ·
Replies
3
Views
2K
Undergrad Quantum Kinetic Energy of Neutrons, Protons and Electrons
  • · Replies 5 ·
Replies
5
Views
2K
Graduate Landau's Maximum Mass Limit Derivation in Shapiro & Teukolsky (1983)
  • · Replies 23 ·
Replies
23
Views
3K