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.

Short Answer

Expert verified

(a) The chemical potential will varyNC=g0cϵCϵ-ϵCeϵ-ϵF/kT+1dϵ

(b) The number of conduction electronsNCg0cπ2(kT)3/2e-ϵC-μ/kT

(c) The valence bond isNv=g0vπ2e-μ-ϵv/kT(kT)3/2

(d) The chemical potential isμ=ϵC+ϵv2-kT2lng0cg0v

(e) The shift for silicon isμshift=-0.0118eV

Step by step solution

01

Part(a) Step 1: Given information

We have been given that g(ϵ)=g0cϵ-ϵC

02

Part(a) Step 2: Given information

The solution is as follows:

NC=ϵCg(ϵ)n¯FDdϵ

NC=g0cϵCϵ-ϵCeϵ-ϵF/kT+1dϵ

03

Part(b) Step 1: Given information

We have been given thatπ2

04

Part(b) Step 2: Simplify

The numbers of electrons in the conduction

0xe-xdx=π2

NCg0cπ2(kT)3/2e-ϵC-μ/kT

05

Part(c) Step 1: GIven information

We have been given that NCV

06

Part(c) Step 2: Simplify

The solution is as follows:

n¯FD=1e(ϵ-μ)/kT+1g(ϵ)=g0vϵv-ϵ

Nv=g0vπ2e-μ-ϵv/kT(kT)3/2

07

Part (d) Step 1: Given information

We have been givenNT3/2e-c/T

08

Part(d) Step 2:Simplify

The temperature increases

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

=6.328×10-26m3

09

Given information

We have been given thatNCV

10

Simplify

The steps are given below

NCV=2m-3=28.00×10-26m3e-Δϵ/(0.052eV)

Δϵ=3.0eV

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Most popular questions from this chapter

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?

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.

(a) Estimate (roughly) the total power radiated by your body, neglecting any energy that is returned by your clothes and environment. (Whatever the color of your skin, its emissivity at infrared wavelengths is quite close to 1; almost any nonmetal is a near-perfect blackbody at these wavelengths.)

(b) Compare the total energy radiated by your body in one day (expressed in kilocalories) to the energy in the food you cat. Why is there such a large discrepancy?

(c) The sun has a mass of 2×1030kgand radiates energy at a rate of 3.9×1026watts. Which puts out more power per units mass-the sun or your body?

Explain in some detail why the three graphs in Figure 7.28 all intercept the vertical axis in about the same place, whereas their slopes differ considerably.

For a system of fermions at room temperature, compute the probability of a single-particle state being occupied if its energy is

(a) 1eVless than μ

(b) 0.01eVless than μ

(c) equal to μ

(d) 0.01eVgreater than μ

(e) 1eVgreater thanμ

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