The previous two problems dealt with pure semiconductors, also called intrinsic semiconductors. Useful semiconductor devices are instead made from doped semiconductors, which contain substantial numbers of impurity atoms. One example of a doped semiconductor was treated in Problem 7.5. Let us now consider that system again. (Note that in Problem 7.5 we measured all energies relative to the bottom of the conduction band, Ee. We also neglected the distinction between g0and g0c; this simplification happens to be ok for conduction electrons in silicon.)

(a) Calculate and plot the chemical potential as afunction of temperature, for silicon doped with 1017phosphorus atoms per cm3(as in Problem 7.5). Continue to assume that the conduction electrons can be treated as an ordinary ideal gas.

(b) Discuss whether it is legitimate to assume for this system that the conduction electrons can be treated asan ordinary ideal gas, as opposed to a Fermi gas. Give some numerical examples.

(c)Estimate the temperature at which the number of valence electrons excitedto the conduction band would become comparable to the number ofconduction electrons from donor impurities. Which source of conductionelectrons is more important at room temperature?

Short Answer

Expert verified

(a). The chemical potential as a function of temperature is:μI=-tln2t3/20.0036xwherex=1-2eI/kTvQNd2V

And the plot of chemical potential as a function of temperature is

(b). Since, ϵ-μkT3IkT=3×1.6955. The approximate Boltzmann distribution should be accurate.

(c). The temperature at which the number of valence electrons excitedto the conduction band would become comparable is T=520K.

Step by step solution

01

Part(a): Step 1: Given information:

We have been given silicon doped with phosphorus atoms.

02

Part(a): Step 2: Explanation

Chemical potential is given byμ=-kTlnVZintNcvQ

Due to two spin states μ=-kTln2VNcvQ

Ratio of Conduction electrons to number of doner atoms is NcNd=x=1-2eI/kTvQNd2V

where μ=-kTln2VxNdvQand x=1-2eI/kTvQNd2V

Let t=kTI

Therefore Quantum volume vQ=h22πmI3/21t3/2

Putting the vlaues of universal constants m,handI.vQ=6.626×10-34J·s22π9.11×10-31kg0.044×1.6×10-19J3/21t3/2=3.6×10-26t-3/2

Also it is known NdV=1×1023m3

EvalutingμI=-tln2x1×1023m33.6×10-26t-3/2

ThereforeμI=-tln2t3/20.0036xandx=1-(0.0036)e1/tt3/2.

03

Part(a): Step 3: Graph

Plotting a graph between μI

04

Part(b): Step 1: Given information

We have to find whether the conduction elements can be treated as an ordinary ideal gas.

05

Part(b): Step 2: Explanation

Considering the denominator of Fermi Dirac that is much greater than 1 we treat it as gas.

Therefore energies of the conduction band ϵ-μkT

The difference between edge energy of conduction band is 3, therefore localid="1650464758608" ϵ-μ3I.

Solving IkT=0.044eV0.026eV=1.695

ϵ-μkT3IkT=3×1.6955

Therefore the value of exponential e5150which is much greater than 1.

Therefore approximating the Fermi Dirac distribution by Boltzmann distribution should be accurate.

06

Part(c): Step 1: Given Information

We have to find out the temperature for which number of valence electrons excited to the conduction band would become comparable to the number of conduction electrons from donor impurities.

07

Part(c): Step 2: Explanation

Saturation point of number of conduction electrons1017Patoms percm3

i.eNdV=1×1023m3

For temperature NCV=2vQe-Δϵ/2kT

Let this expression be equal to 1023; Solving-Δϵ2kT=lnvQNC2V

1T=-2kΔϵlnvQNC2V

Substituting 1T=-28.62×10-5eV1.11eVlnvQNC2V

Quantum volume is given by vQ=6.626×10-34J·s22π9.11×10-31kg1.38×10-23J/K3/21T3/2

=3.6×10-20T-3/2

Therefore

1T=-1.553×10-4ln(0.0018)T-3/2

08

Part(c): Step 3: Graph

Intersection in graph occurs at T=520K

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Most popular questions from this chapter

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.

Evaluate the integral in equation N=2π2πmh23/2V0ϵdϵeϵ/kT-1numerically, to confirm the value quoted in the text.

For a brief time in the early universe, the temperature was hot enough to produce large numbers of electron-positron pairs. These pairs then constituted a third type of "background radiation," in addition to the photons and neutrinos (see Figure 7.21). Like neutrinos, electrons and positrons are fermions. Unlike neutrinos, electrons and positrons are known to be massive (ea.ch with the same mass), and each has two independent polarization states. During the time period of interest, the densities of electrons and positrons were approximately equal, so it is a good approximation to set the chemical potentials equal to zero as in Figure 7.21. When the temperature was greater than the electron mass times c2k, the universe was filled with three types of radiation: electrons and positrons (solid arrows); neutrinos (dashed); and photons (wavy). Bathed in this radiation were a few protons and neutrons, roughly one for every billion radiation particles. the previous problem. Recall from special relativity that the energy of a massive particle is ϵ=(pc)2+mc22.

(a) Show that the energy density of electrons and positrons at temperature Tis given by

u(T)=0x2x2+mc2/kT2ex2+mc2/kT2+1dx;whereu(T)=0x2x2+mc2/kT2ex2+mc2/kT2+1dx

(b) Show that u(T)goes to zero when kTmc2, and explain why this is a

reasonable result.

( c) Evaluate u(T)in the limit kTmc2, and compare to the result of the

the previous problem for the neutrino radiation.

(d) Use a computer to calculate and plot u(T)at intermediate temperatures.

(e) Use the method of Problem 7.46, part (d), to show that the free energy

density of the electron-positron radiation is

FV=-16π(kT)4(hc)3f(T);wheref(T)=0x2ln1+e-x2+mc2/kT2dx

Evaluate f(T)in both limits, and use a computer to calculate and plot f(T)at intermediate

temperatures.

(f) Write the entropy of the electron-positron radiation in terms of the functions

uTand f(T). Evaluate the entropy explicitly in the high-T limit.

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

Consideracollectionof10,000atomsofrubidium-87,confinedinsideaboxofvolume(10-5m)3.(a)Calculateε0,theenergyofthegroundstate.(Expressyouranswerinbothjoulesandelectron-volts.)(b) Calculate the condensation temperature, and comparekTctoϵ0. (c)SupposethatT=0.9Tc.Howmanyatomsareinthegroundstate?Howcloseisthechemicalpotentialtotheground-stateenergy?Howmanyatomsareineachofthe(threefold-degenerate)firstexcitedstates?(d)Repeatparts(b)and(c)forthecaseof106atoms,confinedtothesamevolume.Discusstheconditionsunderwhichthenumberofatomsinthegroundstatewillbemuchgreaterthanthenumberinthefirstexcitedstate.

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