/*! This file is auto-generated */ .wp-block-button__link{color:#fff;background-color:#32373c;border-radius:9999px;box-shadow:none;text-decoration:none;padding:calc(.667em + 2px) calc(1.333em + 2px);font-size:1.125em}.wp-block-file__button{background:#32373c;color:#fff;text-decoration:none} Q. 7.34 In a real semiconductor, the den... [FREE SOLUTION] | 91影视

91影视

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()=g0c-cwhere 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,,candg0cSimplify this expression as much as possible, assuming c-kT.

(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 -vkT.

(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 in碌 for silicon at room temperature.

Short Answer

Expert verified

(a) The chemical potential will varyNC=g0cC-Ce-F/kT+1d

(b) The number of conduction electronsNCg0c2(kT)3/2e-C-/kT

(c) The valence bond isNv=g0v2e--v/kT(kT)3/2

(d) The chemical potential is=C+v2-kT2lng0cg0v

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

Step by step solution

01

Part(a) Step 1: Given information

We have been given that g()=g0c-C

02

Part(a) Step 2: Given information

The solution is as follows:

NC=Cg()nFDd

NC=g0cC-Ce-F/kT+1d

03

Part(b) Step 1: Given information

We have been given that2

04

Part(b) Step 2: Simplify

The numbers of electrons in the conduction

0xe-xdx=2

NCg0c2(kT)3/2e-C-/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:

nFD=1e(-)/kT+1g()=g0vv-

Nv=g0v2e--v/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=6.62610-34Js229.1110-31kg1.3810-23J/K(350K)3/2

=6.32810-26m3

09

Given information

We have been given thatNCV

10

Simplify

The steps are given below

NCV=2m-3=28.0010-26m3e-/(0.052eV)

=3.0eV

Unlock Step-by-Step Solutions & Ace Your Exams!

  • Full Textbook Solutions

    Get detailed explanations and key concepts

  • Unlimited Al creation

    Al flashcards, explanations, exams and more...

  • Ads-free access

    To over 500 millions flashcards

  • Money-back guarantee

    We refund you if you fail your exam.

Over 30 million students worldwide already upgrade their learning with 91影视!

One App. One Place for Learning.

All the tools & learning materials you need for study success - in one app.

Get started for free

Most popular questions from this chapter

In analogy with the previous problem, consider a system of identical spin0bosonstrapped in a region where the energy levels are evenly spaced. Assume that Nis a large number, and again let qbe the number of energy units.

(a) Draw diagrams representing all allowed system states from q=0up to q=6.Instead of using dots as in the previous problem, use numbers to indicate the number of bosons occupying each level.

(b) Compute the occupancy of each energy level, for q=6. Draw a graph of the occupancy as a function of the energy at each level.

(c) Estimate values of and Tthat you would have to plug into the Bose-Einstein distribution to best fit the graph of part(b).

(d) As in part (d) of the previous problem, draw a graph of entropy vs energy and estimate the temperature at q=6from this graph.

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?

Problem 7.69. If you have a computer system that can do numerical integrals, it's not particularly difficult to evaluate forT>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=/kTc,andx=/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 , holding Tfixed, to find the precise value of for T=2Tc. Repeat for values of T/Tcranging from 1.2up to 3.0, in increments of 0.2. Plot a graph of as a function of temperature.

Use the formula P=-(U/V)S,N to show that the pressure of a photon gas is 1/3 times the energy density (U/V). Compute the pressure exerted by the radiation inside a kiln at 1500 K, and compare to the ordinary gas pressure exerted by the air. Then compute the pressure of the radiation at the centre of the sun, where the temperature is 15 million K. Compare to the gas pressure of the ionised hydrogen, whose density is approximately 105 kg/m3.

The results of the previous problem can be used to explain why the current temperature of the cosmic neutrino background (Problem 7.48) is 1.95 K rather than 2.73 K. Originally the temperatures of the photons and the neutrinos would have been equal, but as the universe expanded and cooled, the interactions of neutrinos with other particles soon became negligibly weak. Shortly thereafter, the temperature dropped to the point where kT/c2 was no longer much greater than the electron mass. As the electrons and positrons disappeared during the next few minutes, they "heated" the photon radiation but not the neutrino radiation.

(a) Imagine that the universe has some finite total volume V, but that V is increasing with time. Write down a formula for the total entropy of the electrons, positrons, and photons as a function of V and T, using the auxiliary functions u(T) and f(T) introduced in the previous problem. Argue that this total entropy would have ben conserved in the early universe, assuming that no other species of particles interacted with these.

(b) The entropy of the neutrino radiation would have been separately conserved during this time period, because the neutrinos were unable to interact with anything. Use this fact to show that the neutrino temperature Tv and the photon temperature T are related by

TT32445+u(T)+f(T)=constant

as the universe expands and cools. Evaluate the constant by assuming that T=Tv when the temperatures are very high.

(c) Calculate the ratio T/Tv, in the limit of low temperature, to confirm that the present neutrino temperature should be 1.95 K.

(d) Use a computer to plot the ratio T/Tv, as a function of T, for kT/mc2ranging from 0 to 3.*

See all solutions

Recommended explanations on Physics Textbooks

View all explanations

What do you think about this solution?

We value your feedback to improve our textbook solutions.

Study anywhere. Anytime. Across all devices.