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Consider a free Fermi gas in two dimensions, confined to a square area A=L2

(a) Find the Fermi energy (in terms of Nand A), and show that the average energy of the particles is F2.

(b) Derive a formula for the density of states. You should find that it is a constant, independent of .

(c) Explain how the chemical potential of this system should behave as a function of temperature, both when role="math" localid="1650186338941" kTFand when Tis much higher.

(d) Because gis a constant for this system, it is possible to carry out the integral 7.53 for the number of particles analytically. Do so, and solve for μas a function of N. Show that the resulting formula has the expected qualitative behavior.

(e) Show that in the high-temperature limit, kTF, the chemical potential of this system is the same as that of an ordinary ideal gas.

Short Answer

Expert verified

(a) Fermi energy is, 12NFand the average energy relation is given below.

(b) Density of states is, g=NF

(c) As the density state is constant, so the behavior of chemical properties is the same as the Fermi-Dirac distribution i.e. it will decrease continuously.

(d) Value of μis, μ=kTlneFkT-1

(e) Since, μ=-kTlnAN×2lQ2. Therefore, we can say that the chemical potential of this system is the same as that of an ordinary ideal gas.

Step by step solution

01

Part(a) Step 1: Given information

We have been given that,

A=L2

02

Part (a) Step 2: Simplify

In two dimensional case,

N=20nmax0π/2ndndθ=π2nmax2

We know that,

F=h2nmax28mL2=h28mA×2NπF=h24πmAN

Now, we can find the total energy U,

U=20nmax0π2ndndθ=π2nmax2U=0Fπ8mAh28mAh212dU=0F4πmAh2dU=0FNFdU=12NF

So, we can easily get average energy of the particles is UN=F2

03

Part (b) Step 1: Given information

We need to find out the density of states.

04

Part (b) Step 2: Simplify

From part (a),

Density of states is,

g=NF

That is independent of

05

Part (c) Step 1: Given information

We need to find out behavior of chemical properties

06

Part (c) Step 2: Simplify

Since the density of state is constant, the behavior of the chemical potential is the same as that of the Fermi-Dirac distribution. As we know that Fermi-Dirac distribution has some symmetrical property but when the energy difference from μis higher than the chemical potential, it gets broken because the occupancy is zero when <0. So, the electrons with energy less than the Fermi energy are excited to a higher level than the Fermi energy with broken symmetry, which means that the number of electron loss with energy <Fis lower than the number of electron gain with energy >F.

To be sensible with the difference in no. of electrons, chemical potential should move i.e. Fermi-Dirac distribution has to move totally. As the number of electrons with energy >Fis larger than <F, so Fermi-Dirac distribution has to move on the left side with fixed F, which means that the chemical potential decreases. When the temperature slightly grows up, then the difference in the number of electrons also grows up. So, the chemical potential will decrease continuously and at some point, it will have a negative value.

07

Part (d) Step 1: Given information

We need to find out value ofμ

08

Part (d) Step 2: Simplify

Since g()is a constant, we can analytically integrate the equation,

N=0g1e-μkT+1d=NF0e--μkT1+e--μkTd=NF-kTln1+e--μkT=0==NFkTln1+eμkT

From this,

μ=kTlnFkT-1=FwherekTFkTlnFkTwherekTF

The second case is approximately and it will be negative value.

09

Part(e) Step 1: Given information

We need to find out that the chemical properties of this system is the same as that of an ordinary ideal gas

10

Part (e) Step 2: Simplify 

From the answer of part (d),

μ=kTlnFkT=kTlnAN×4πmkTh2=-kTlnAN×2lQ2

It seems to be the same form with the equation of chemical potential of an ordinary ideal gas.

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Most popular questions from this chapter

For a system obeying Boltzmann statistics, we know what μis from Chapter 6. Suppose, though, that you knew the distribution function (equation 7.31) but didn't know μ. You could still determine μ by requiring that the total number of particles, summed over all single-particle states, equal N. Carry out this calculation, to rederive the formula μ=-kTlnZ1/N. (This is normally how μ is determined in quantum statistics, although the math is usually more difficult.)

The Sommerfeld expansion is an expansion in powers of kTεF, which is assumed to be small. In this section I kept all terms through order kTεF2, omitting higher-order terms. Show at each relevant step that the term proportional to localid="1650117451748" T3is zero, so that the next nonvanishing terms in the expansions forlocalid="1650117470867" μand localid="1650117476821" Uare proportional to localid="1650117458596" T4. (If you enjoy such things, you might try evaluating the localid="1650117464980" T4terms, possibly with the aid of a computer algebra program.)

Problem 7.69. If you have a computer system that can do numerical integrals, it's not particularly difficult to evaluate μforT>Tc.

(a) As usual when solving a problem on a computer, it's best to start by putting everything in terms of dimensionless variables. So define t=T/Tc,c=μ/kTc,andx=ϵ/kTc. Express the integral that defines , equation 7.22, in terms of these variables. You should obtain the equation

2.315=0xdxe(x-c)/t-1

(b) According to Figure

the correct value of cwhen T=2Tcis approximately -0.8. Plug in these values and check that the equation above is approximately satisfied.

(c) Now vary μ, holding Tfixed, to find the precise value of μfor T=2Tc. Repeat for values of T/Tcranging from 1.2up to 3.0, in increments of 0.2. Plot a graph of μas a function of temperature.

A star that is too heavy to stabilize as a white dwarf can collapse further to form a neutron star: a star made entirely of neutrons, supported against gravitational collapse by degenerate neutron pressure. Repeat the steps of the previous problem for a neutron star, to determine the following: the mass radius relation; the radius, density, Fermi energy, and Fermi temperature of a one-solar-mass neutron star; and the critical mass above which a neutron star becomes relativistic and hence unstable to further collapse.

The speed of sound in copper is 3560m/s. Use this value to calculate its theoretical Debye temperature. Then determine the experimental Debye temperature from Figure 7.28, and compare.

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