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


Fill in the steps to derive equations 7.112and7.117.

Consider any two internal states, s1 and s2, of an atom. Let s2 be the higher-energy state, so that Es2-Es1=ϵ for some positive constant. If the atom is currently in state s2, then there is a certain probability per unit time for it to spontaneously decay down to state s1, emitting a photon with energy e. This probability per unit time is called the Einstein A coefficient:

A = probability of spontaneous decay per unit time.

On the other hand, if the atom is currently in state s1 and we shine light on it with frequency f=ϵ/h, then there is a chance that it will absorb photon, jumping into state s2. The probability for this to occur is proportional not only to the amount of time elapsed but also to the intensity of the light, or more precisely, the energy density of the light per unit frequency, u(f). (This is the function which, when integrated over any frequency interval, gives the energy per unit volume within that frequency interval. For our atomic transition, all that matters is the value of u(f)atf=ϵ/h) The probability of absorbing a photon, per unit time per unit intensity, is called the Einstein B coefficient:

B=probability of absorption per unit timeu(f)

Finally, it is also possible for the atom to make a stimulated transition from s2down to s1, again with a probability that is proportional to the intensity of light at frequency f. (Stimulated emission is the fundamental mechanism of the laser: Light Amplification by Stimulated Emission of Radiation.) Thus we define a third coefficient, B, that is analogous to B:

B'=probability of stimulated emission per unit timeu(f)

As Einstein showed in 1917, knowing any one of these three coefficients is as good as knowing them all.

(a) Imagine a collection of many of these atoms, such that N1 of them are in state s1 and N2 are in state s2. Write down a formula for dN1/dt in terms of A, B, B', N1, N2, and u(f).

(b) Einstein's trick is to imagine that these atoms are bathed in thermal radiation, so that u(f) is the Planck spectral function. At equilibrium, N1and N2 should be constant in time, with their ratio given by a simple Boltzmann factor. Show, then, that the coefficients must be related by

B'=BandAB=8πhf3c3

Compute the quantum volume for an N2molecule at room temperature, and argue that a gas of such molecules at atmospheric pressure can be

treated using Boltzmann statistics. At about what temperature would quantum statistics become relevant for this system (keeping the density constant and pretending that the gas does not liquefy)?

Use the results of this section to estimate the contribution of conduction electrons to the heat capacity of one mole of copper at room temperature. How does this contribution compare to that of lattice vibrations, assuming that these are not frozen out? (The electronic contribution has been measured at low temperatures, and turns out to be about40% more than predicted by the free electron model used here.)

Starting from the formula for CV derived in Problem 7.70(b), calculate the entropy, Helmholtz free energy, and pressure of a Bose gas for T<Tc. Notice that the pressure is independent of volume; how can this be the case?

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