Question

In what ways are thermal pressure and electron degeneracy similar? How do they differ? In what objects do these forces play a role?

Given that nucleosynthesis discontinues after iron, how are heavier elements formed?

Explain the significance of Supernova 1987. Why was this event so valuable to astronomers?

Just need a short answers.

Answer 1

Particles generally occupy high states of kinetic energy in order to satisfy Pauli Exclusion Principle. This applies to all particles like electrons, protons, and fermions. According to Pauli Exclusion Principle no two identical half-integer spin occupy the same quantum state.

Thermal pressure and electron degeneracy are common according to the concept of degeneracy or following the Pauli’s exclusion principle.

Thermal pressure is generally observed in the field of astrophysics. This term is used to refer dense stellar objects where the quantum mechanical effects become significant. The value of thermal pressure is non zero even at the absolute temperature, thus doesn’t happen with electron degeneracy. Also thermal pressure is independent on temperature unlike electron degeneracy. Thermal pressure helps to maintain the equilibrium of dense stars.