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In Problem 7.28you found the density of states and the chemical potential for a two-dimensional Fermi gas. Calculate the heat capacity of this gas in the limit role="math" localid="1650099524353" kTεF· Also show that the heat capacity has the expected behavior when kTεF. Sketch the heat capacity as a function of temperature.

Short Answer

Expert verified

The heat capacity of the gas in the limit is CV=N(kπ)2T3εF.

The graph of heat capacity as a function of temperature is

Step by step solution

01

Given information

We have been given that the density of states and the chemical potential for a two-dimensional Fermi gas which we have found earlier in Problem 7.28isg(ε)=NεF.

We need to find the heat capacity of this gas in the limit kTεFand show that the heat capacity has the expected behavior when kTεF. Also we need to sketch the heat capacity as a function of temperature.

02

Simplify

The total energy is given by the following integral:

U=0εg(ε)n¯FD(ε)dε (Let this equation be (localid="1650103209259" 1))

We have found the energy density earlier in Problem 7.28such as

localid="1650102270353" g(ε)=NεF

Substitute the value of g(ε)in equation (localid="1650103517684" 1), we get:

U=NεF0εn¯FD(ε)dε

Integrating by parts, we get:

U=NεFε22n¯FD|0-NεF0ε22n¯FDεdε (Let this equation be (2))

If we substitute ε=0, the integral will become zero due to the dependence of the term on ε2and the first term vanishes.

The equation (2) reduces to :

U=-NεF0ε22n¯FDεdε (Let this equation be (3))

We know that n¯FD=1e(e-μ)kT+1

Taking derivative with respect to ε, we get:

localid="1650103912932" n¯FDε=1e(ε-μ)kT+1ε

n¯FDε=-1kTe(ε-μ)kT(e(ε-μ)kT+1)2

Let (ε-μ)kT=x, then we can write as:

dx=dεkT

We also need to change the boundaries of integration, so:

ε x

ε0 x-μkT

As kTμ, we can put -as the lower limit of integration.

The integral in equation (3) will become:

U=N2εF-ε2ex(ex+1)2dx (Let this equation be (localid="1650114310341" 4))

03

finding the values of integrals

Now expanding ε2about μusing Taylor series, we get:

ε2=μ2+2μ(ε-μ)x+(ε-μ)x2ε2=μ2+2μ(kTx)+(kTx)2

By substituting the value of in equation (4), we get three integrals say I1,I2,I3

The equation (4) will become:

U=N2εF[I1+I2+I3] (Let this equation be (5))

where,

I1=μ2-ex(ex+1)2dxI2=2kTμ-xex(ex+1)2dxI3=(kT)2-x2ex(ex+1)2dx

Simplifying the integrals I1,I2,I3, we get:

I1=μ2

The second integral is odd integral and the limits of integration are from to , so this integral is simply zero.

I2=0

I3=(kT)2mfrac23=(kTπ)23

Substitute the values of in equation (5), we get:

U=N2εFμ2+(kTπ)23

Let μ=εF, we get:

U=N2εFεF2+(kTπ)23U=NεF2+N(kTπ)26εF

The heat capacity is the partial derivative of with respect to the temperature, that is:

CV=UTCV=NεF2+N(kTπ)26εFTCV=N(kπ)2T3εF

04

Graph

The graph of the heat capacity as a function of temperature is linear, where the slope of the line is Slope=N(kπ)23εF.

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Most popular questions from this chapter

Although the integrals (7.53and 7.54) forNand Ucannot be

carried out analytically for all T, it's not difficult to evaluate them numerically

using a computer. This calculation has little relevance for electrons in metals (for

which the limit kT<<EFis always sufficient), but it is needed for liquid H3eand

for astrophysical systems like the electrons at the center of the sun.

(a) As a warm-up exercise, evaluate theNintegral (7.53) for the casekT=εF

and μ=0, and check that your answer is consistent with the graph shown

above. (Hint: As always when solving a problem on a computer, it's best to

first put everything in terms of dimensionless variables. So let t=kTεFrole="math" localid="1649996205331" ,c=μεF

, and x=εkT. Rewrite everything in terms of these variables,

and then put it on the computer.)

(b) The next step is to varyμ holdingT fixed, until the integral works out to

the desired value,N. Do this for values of kTεFranging from 0.1 up to 2,

and plot the results to reproduce Figure7.16. (It's probably not a good idea

to try to use numerical methods when kTεF is much smaller than 0.1, since

you can start getting overflow errors from exponentiating large numbers.

But this is the region where we've already solved the problem analytically.)

(c) Plug your calculated values ofµ into the energy integral (7.54), and evaluate

that integral numerically to obtain the energy as a function of temperature

forkTup to 2εF Plot the results, and evaluate the slope to obtain the

heat capacity. Check that the heat capacity has the expected behavior at

both low and high temperatures.

For a system of bosons at room temperature, compute the average occupancy of a single-particle state and the probability of the state containing 0,1,2,3bosons, if the energy of the state is

(a) 0.001eVgreater than μ

(b) 0.01eVgreater than μ

(c) 0.1eVgreater than μ

(d) 1eVgreater than μ

The sun is the only star whose size we can easily measure directly; astronomers therefore estimate the sizes of other stars using Stefan's law.

(a) The spectrum of Sirius A, plotted as a function of energy, peaks at a photon energy of2.4eV, while Sirius A is approximately 24times as luminous as the sun. How does the radius of Sirius A compare to the sun's radius?

(b) Sirius B, the companion of Sirius A (see Figure 7.12), is only role="math" localid="1647765883396" 3%as luminous as the sun. Its spectrum, plotted as a function of energy, peaks at about7eV. How does its radius compare to that of the sun?

(c) The spectrum of the star Betelgeuse, plotted as a function of energy, peaks at a photon energy of 0.8eV, while Betelgeuse is approximately10,000times as luminous as the sun. How does the radius of Betelgeuse compare to the sun's radius? Why is Betelgeuse called a "red supergiant"?

Consider a Bose gas confined in an isotropic harmonic trap, as in the previous problem. For this system, because the energy level structure is much simpler than that of a three-dimensional box, it is feasible to carry out the sum in equation 7.121 numerically, without approximating it as an integral.*

(a) Write equation 7.121 for this system as a sum over energy levels, taking degeneracy into account. Replace Tandμwith the dimensionless variables t=kT/hfandc=μ/hf.

(b) Program a computer to calculate this sum for any given values of tandc. Show that, for N=2000, equation 7.121 is satisfied at t=15provided that c=-10.534. (Hint: You'll need to include approximately the first 200 energy levels in the sum.)

(c) For the same parameters as in part (b), plot the number of particles in each energy level as a function of energy.

(d) Now reduce tto 14 , and adjust the value of cuntil the sum again equals 2000. Plot the number of particles as a function of energy.

(e) Repeat part (d) for t=13,12,11,and10. You should find that the required value of cincreases toward zero but never quite reaches it. Discuss the results in some detail.

The tungsten filament of an incandescent light bulb has a temperature of approximately 3000K. The emissivity of tungsten is approximately 13, and you may assume that it is independent of wavelength.

(a) If the bulb gives off a total of 100watts, what is the surface area of its filament in square millimetres?

(b) At what value of the photon energy does the peak in the bulb's spectrum occur? What is the wavelength corresponding to this photon energy?

(c) Sketch (or use a computer to plot) the spectrum of light given off by the filament. Indicate the region on the graph that corresponds to visible wavelengths, between400and700nm.

(d) Calculate the fraction of the bulb's energy that comes out as visible light. (Do the integral numerically on a calculator or computer.) Check your result qualitatively from the graph of part (c).

( e) To increase the efficiency of an incandescent bulb, would you want to raise or lower the temperature? (Some incandescent bulbs do attain slightly higher efficiency by using a different temperature.)

(f) Estimate the maximum possible efficiency (i.e., fraction of energy in the visible spectrum) of an incandescent bulb, and the corresponding filament temperature. Neglect the fact that tungsten melts at 3695K.

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