When the attractive forces of the ions in a crystal are taken into account, the allowed electron energies are no longer given by the simple formula 7.36; instead, the allowed energies are grouped into bands, separated by gaps where there are no allowed energies. In a conductor the Fermi energy lies within one of the bands; in this section we have treated the electrons in this band as "free" particles confined to a fixed volume. In an insulator, on the other hand, the Fermi energy lies within a gap, so that at T = 0 the band below the gap is completely occupied while the band above the gap is unoccupied. Because there are no empty states close in energy to those that are occupied, the electrons are "stuck in place" and the material does not conduct electricity. A semiconductor is an insulator in which the gap is narrow enough for a few electrons to jump across it at room temperature. Figure 7 .17 shows the density of states in the vicinity of the Fermi energy for an idealized semiconductor, and defines some terminology and notation to be used in this problem.

(a) As a first approximation, let us model the density of states near the bottom of the conduction band using the same function as for a free Fermi gas, with an appropriate zero-point: g(ϵ)=g0ϵ-ϵc, where go is the same constant as in equation 7.51. Let us also model the density of states near the top

Figure 7.17. The periodic potential of a crystal lattice results in a densityof-states function consisting of "bands" (with many states) and "gaps" (with no states). For an insulator or a semiconductor, the Fermi energy lies in the middle of a gap so that at T = 0, the "valence band" is completely full while the-"conduction band" is completely empty. of the valence band as a mirror image of this function. Explain why, in this approximation, the chemical potential must always lie precisely in the middle of the gap, regardless of temperature.

(b) Normally the width of the gap is much greater than kT. Working in this limit, derive an expression for the number of conduction electrons per unit volume, in terms of the temperature and the width of the gap.

(c) For silicon near room temperature, the gap between the valence and conduction bands is approximately 1.11 eV. Roughly how many conduction electrons are there in a cubic centimeter of silicon at room temperature? How does this compare to the number of conduction electrons in a similar amount of copper?

( d) Explain why a semiconductor conducts electricity much better at higher temperatures. Back up your explanation with some numbers. (Ordinary conductors like copper, on the other hand, conduct better at low temperatures.) (e) Very roughly, how wide would the gap between the valence and conduction bands have to be in order to consider a material an insulator rather than a semiconductor?

Short Answer

Expert verified

(a). The chemical potential in the middle is

NC=2VvQe-Δϵ/2kT

(b). The number of the conduction electrons per unit volume

g(ε)=g0ε-ε

(c). The conduction electrons are there in a cubic centimeter is

NCV=1.18×1016m-3

(d) At the room temperature NT3/2e-c/T

Step by step solution

01

part(a) Step 1:given information

we have been given thatNC=ϵCg(ϵ)n¯FDdϵ

02

part(a) Step 2: Simplify

energy distribution is given by:

n¯FD=1eϵ-ϵF/kT+1g(ϵ)=g0ϵ-ϵ

NCg0ϵCϵ-ϵCe-ϵ-ϵC/kTe-ϵC-ϵF/kTdϵ

03

part(b) Step 1: Given information

we have been given that at zero temperature there will be some electrons in the conductors

04

part(b) Step 2: Explanation

a point ofϵ=μ, so we can conclude that the probability of state atϵbeing occupied is equals the probability of state

05

part(c) step 1: given information

we have been given thatvQ=6.626×10-34J·s22π9.11×10-31kg1.38×10-23J/K(300K)3/2

06

part(c) Step 2: Simplify

at room temperature

NCV=28.00×10-26m3e-1.778×10-19J/21.38×10-23J/K(300K)

electrons in copper is:

NCV=8.47×1028m-3

07

part(d) Step 1: given information

we have been given thatNT3/2e-c/T

08

part(d) step 2: simplify

The terms we get:

vQ=6.626×10-34J·s22π9.11×10-31kg1.38×10-23J/K(350K)3/2

therefore volume is

NCV=26.328×10-26m3e-1.778×10-19J/21.38×10-23J/K(350K)

09

Part(e) Step 1: Given information

The number of electrons per unit volume

NCV=28.00×10-26m3e-Δϵ/(0.052eV)

10

Part(e) Step 2:Simplify

The width of the gap is measured

NCV=28.00×10-26m3e-Δϵ/(0.052eV)

e-Δϵ/(0.052eV)=8.00×10-26

Δϵ=3.0eV

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Most popular questions from this chapter

An atomic nucleus can be crudely modeled as a gas of nucleons with a number density of 0.18fm-3(where 1fm=10-15m). Because nucleons come in two different types (protons and neutrons), each with spin 1/2, each spatial wavefunction can hold four nucleons. Calculate the Fermi energy of this system, in MeV. Also calculate the Fermi temperature, and comment on the result.

Each atom in a chunk of copper contributes one conduction electron. Look up the density and atomic mass of copper, and calculate the Fermi energy, the Fermi temperature, the degeneracy pressure, and the contribution of the degeneracy pressure to the bulk modulus. Is room temperature sufficiently low to treat this system as a degenerate electron gas?

In a real semiconductor, the density of states at the bottom of the conduction band will differ from the model used in the previous problem by a numerical factor, which can be small or large depending on the material. Let us, therefore, write for the conduction band g(ϵ)=g0cϵ-ϵcwhere g0cis a new normalization constant that differs from g0by some fudge factor. Similarly, write gat the top of the valence band in terms of a new normalization constant g0v.

(a) Explain why, if g0vg0c, the chemical potential will now vary with temperature. When will it increase, and when will it decrease?

(b) Write down an expression for the number of conduction electrons, in terms of T,μ,candg0cSimplify this expression as much as possible, assuming ϵc-μkT.

(c) An empty state in the valence band is called a hole. In analogy to part (b), write down an expression for the number of holes, and simplify it in the limit μ-ϵvkT.

(d) Combine the results of parts (b) and (c) to find an expression for the chemical potential as a function of temperature.

(e) For silicon, g0cg0=1.09andg0vg0=0.44*.Calculate the shift inµ for silicon at room temperature.

A white dwarf star (see Figure 7.12) is essentially a degenerate electron gas, with a bunch of nuclei mixed in to balance the charge and to provide the gravitational attraction that holds the star together. In this problem you will derive a relation between the mass and the radius of a white dwarf star, modeling the star as a uniform-density sphere. White dwarf stars tend to be extremely hot by our standards; nevertheless, it is an excellent approximation in this problem to set T=0.

(a) Use dimensional analysis to argue that the gravitational potential energy of a uniform-density sphere (mass M, radius R) must equal

Ugrav=-(constant)GM2R

where (constant) is some numerical constant. Be sure to explain the minus sign. The constant turns out to equal 3/5; you can derive it by calculating the (negative) work needed to assemble the sphere, shell by shell, from the inside out.

(b) Assuming that the star contains one proton and one neutron for each electron, and that the electrons are nonrelativistic, show that the total (kinetic) energy of the degenerate electrons equals

Ukinetic=(0.0086)h2M53memp53R2

Figure 7.12. The double star system Sirius A and B. Sirius A (greatly overexposed in the photo) is the brightest star in our night sky. Its companion, Sirius B, is hotter but very faint, indicating that it must be extremely small-a white dwarf. From the orbital motion of the pair we know that Sirius B has about the same mass as our sun. (UCO /Lick Observatory photo.)

( c) The equilibrium radius of the white dwarf is that which minimizes the total energy Ugravity+Ukinetic· Sketch the total energy as a function of R, and find a formula for the equilibrium radius in terms of the mass. As the mass increases, does the radius increase or decrease? Does this make sense?

( d) Evaluate the equilibrium radius for M=2×1030kg, the mass of the sun. Also evaluate the density. How does the density compare to that of water?

( e) Calculate the Fermi energy and the Fermi temperature, for the case considered in part (d). Discuss whether the approximation T = 0 is valid.

(f) Suppose instead that the electrons in the white dwarf star are highly relativistic. Using the result of the previous problem, show that the total kinetic energy of the electrons is now proportional to 1 / R instead of 1R2• Argue that there is no stable equilibrium radius for such a star.

(g) The transition from the nonrelativistic regime to the ultra relativistic regime occurs approximately where the average kinetic energy of an electron is equal to its rest energy, mc2Is the nonrelativistic approximation valid for a one-solar-mass white dwarf? Above what mass would you expect a white dwarf to become relativistic and hence unstable?

Sometimes it is useful to know the free energy of a photon gas.

(a) Calculate the (Helmholtz) free energy directly from the definition

(Express the answer in terms of T' and V.)

(b) Check the formula S=-(F/T)Vfor this system.

(c) Differentiate F with respect to V to obtain the pressure of a photon gas. Check that your result agrees with that of the previous problem.

(d) A more interesting way to calculate F is to apply the formula F=-kTlnZ separately to each mode (that is, each effective oscillator), then sum over all modes. Carry out this calculation, to obtain

F=8πV(kT)4(hc)30x2ln1-e-xdx

Integrate by parts, and check that your answer agrees with part (a).

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