Repeat the previous problem, taking into account the two independent spin states of the electron. Now the system has two "occupied" states, one with the electron in each spin configuration. However, the chemical potential of the electron gas is also slightly different. Show that the ratio of probabilities is the same as before: The spin degeneracy cancels out of the saha equation.

Short Answer

Expert verified

A system of a single Hydrogen atom/ion, which has two possible states: Unoccupied and occupied. Taking into account the two independent spin states of the electron, now the system has two occupied states one with the electron in each spin configuration.

Step by step solution

01

Unoccupied state:

Energy (ε)=0

Occupation number (n)=0

Gibbs Factor=exp-1KT(ε-nμ)=exp-(0-0.μ)kT=exp(0)=1

02

Singly occupied states:

Energy

Occupation

Degeneracy

Gibbs Factor

The partition function is

ε=-1
03

The probability that the hydrogen atom is ionized is:

Pionized=11+2exp(1+μ)kT

The probability that the hydrogen atom is neutral

Pneutral=2expI+μkT1+2expI+μkT

04

The chemical potential of the electron gas can be written as:

μ=-kTlnVZintNvQWhere Zint=2for the two spin states.

role="math" PionizedPneutral=12expI+μkT=exp-IkT2expμkTμ=-kTlnVZintNvQ=kTlnNvQ2VexpμkT=NvQ2VPionizedPneutral=exp-IkT2NvQ2VPionizedPneutral=VNvQexp-IkT

As T0,vQ,exp-IkT

And PionizedPneutral0,which is what you would expect, if none of the hydrogen atoms are ionized.

role="math" T,vQ0,exp-IkT1PionizedPneutral

i.e., all the hydrogen atoms are ionized andPneutral0

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Most popular questions from this chapter

For a brief time in the early universe, the temperature was hot enough to produce large numbers of electron-positron pairs. These pairs then constituted a third type of "background radiation," in addition to the photons and neutrinos (see Figure 7.21). Like neutrinos, electrons and positrons are fermions. Unlike neutrinos, electrons and positrons are known to be massive (ea.ch with the same mass), and each has two independent polarization states. During the time period of interest, the densities of electrons and positrons were approximately equal, so it is a good approximation to set the chemical potentials equal to zero as in Figure 7.21. When the temperature was greater than the electron mass times c2k, the universe was filled with three types of radiation: electrons and positrons (solid arrows); neutrinos (dashed); and photons (wavy). Bathed in this radiation were a few protons and neutrons, roughly one for every billion radiation particles. the previous problem. Recall from special relativity that the energy of a massive particle is ϵ=(pc)2+mc22.

(a) Show that the energy density of electrons and positrons at temperature Tis given by

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(b) Show that u(T)goes to zero when kTmc2, and explain why this is a

reasonable result.

( c) Evaluate u(T)in the limit kTmc2, and compare to the result of the

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(d) Use a computer to calculate and plot u(T)at intermediate temperatures.

(e) Use the method of Problem 7.46, part (d), to show that the free energy

density of the electron-positron radiation is

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Evaluate f(T)in both limits, and use a computer to calculate and plot f(T)at intermediate

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(f) Write the entropy of the electron-positron radiation in terms of the functions

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N=kTZZμ

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Use these results to show that the standard deviation of Nis

σN=kTN/μ,

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Consider a degenerate electron gas in which essentially all of the electrons are highly relativistic ϵmc2so that their energies are ϵ=pc(where p is the magnitude of the momentum vector).

(a) Modify the derivation given above to show that for a relativistic electron gas at zero temperature, the chemical potential (or Fermi energy) is given by =

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(b) Find a formula for the total energy of this system in terms of N and μ.

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