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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" kTF路 Also show that the heat capacity has the expected behavior when kTF. 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(k)2T3F.

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()=NF.

We need to find the heat capacity of this gas in the limit kTFand show that the heat capacity has the expected behavior when kTF. 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=0g()nFD()d (Let this equation be (localid="1650103209259" 1))

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

localid="1650102270353" g()=NF

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

U=NF0nFD()d

Integrating by parts, we get:

U=NF22nFD|0-NF022nFDd (Let this equation be (2))

If we substitute =0, the integral will become zero due to the dependence of the term on 2and the first term vanishes.

The equation (2) reduces to :

U=-NF022nFDd (Let this equation be (3))

We know that nFD=1e(e-)kT+1

Taking derivative with respect to , we get:

localid="1650103912932" nFD=1e(-)kT+1

nFD=-1kTe(-)kT(e(-)kT+1)2

Let (-)kT=x, then we can write as:

dx=dkT

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

x

0 x-kT

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

The integral in equation (3) will become:

U=N2F-2ex(ex+1)2dx (Let this equation be (localid="1650114310341" 4))

03

finding the values of integrals

Now expanding 2about using Taylor series, we get:

2=2+2(-)x+(-)x22=2+2(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=N2F[I1+I2+I3] (Let this equation be (5))

where,

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

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

I1=2

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

I2=0

I3=(kT)223=(kT)23

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

U=N2F2+(kT)23

Let =F, we get:

U=N2FF2+(kT)23U=NF2+N(kT)26F

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

CV=UTCV=NF2+N(kT)26FTCV=N(k)2T3F

04

Graph

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

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Most popular questions from this chapter

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.

At the center of the sun, the temperature is approximately 107K and the concentration of electrons is approximately 1032 per cubic meter. Would it be (approximately) valid to treat these electrons as a "classical" ideal gas (using Boltzmann statistics), or as a degenerate Fermi gas (with T0 ), or neither?

In addition to the cosmic background radiation of photons, the universe is thought to be permeated with a background radiation of neutrinos (v) and antineutrinos (v-), currently at an effective temperature of 1.95 K. There are three species of neutrinos, each of which has an antiparticle, with only one allowed polarisation state for each particle or antiparticle. For parts (a) through (c) below, assume that all three species are exactly massless

(a) It is reasonable to assume that for each species, the concentration of neutrinos equals the concentration of antineutrinos, so that their chemical potentials are equal: =. Furthermore, neutrinos and antineutrinos can be produced and annihilated in pairs by the reaction

+2

(where y is a photon). Assuming that this reaction is at equilibrium (as it would have been in the very early universe), prove that u =0 for both the neutrinos and the antineutrinos.

(b) If neutrinos are massless, they must be highly relativistic. They are also fermions: They obey the exclusion principle. Use these facts to derive a formula for the total energy density (energy per unit volume) of the neutrino-antineutrino background radiation. differences between this "neutrino gas" and a photon gas. Antiparticles still have positive energy, so to include the antineutrinos all you need is a factor of 2. To account for the three species, just multiply by 3.) To evaluate the final integral, first change to a dimensionless variable and then use a computer or look it up in a table or consult Appendix B. (Hint: There are very few

(c) Derive a formula for the number of neutrinos per unit volume in the neutrino background radiation. Evaluate your result numerically for the present neutrino temperature of 1.95 K.

d) It is possible that neutrinos have very small, but nonzero, masses. This wouldn't have affected the production of neutrinos in the early universe, when me would have been negligible compared to typical thermal energies. But today, the total mass of all the background neutrinos could be significant. Suppose, then, that just one of the three species of neutrinos (and the corresponding antineutrino) has a nonzero mass m. What would mc2 have to be (in eV), in order for the total mass of neutrinos in the universe to be comparable to the total mass of ordinary matter?

Show that when a system is in thermal and diffusive equilibrium with a reservoir, the average number of particles in the system is

N=kTZZ

where the partial derivative is taken at fixed temperature and volume. Show also that the mean square number of particles is

N2=(kT)2Z2Z2

Use these results to show that the standard deviation of Nis

N=kTN/,

in analogy with Problem6.18Finally, apply this formula to an ideal gas, to obtain a simple expression forNin terms ofNDiscuss your result briefly.

The argument given above for why CvTdoes not depend on the details of the energy levels available to the fermions, so it should also apply to the model considered in Problem 7.16: a gas of fermions trapped in such a way that the energy levels are evenly spaced and non-degenerate.

(a) Show that, in this model, the number of possible system states for a given value of q is equal to the number of distinct ways of writing q as a sum of positive integers. (For example, there are three system states for q = 3, corresponding to the sums 3, 2 + 1, and 1 + 1 + 1. Note that 2 + 1 and 1 + 2 are not counted separately.) This combinatorial function is called the number of unrestricted partitions of q, denoted p(q). For example, p(3) = 3.

(b) By enumerating the partitions explicitly, compute p(7) and p(8).

(c) Make a table of p(q) for values of q up to 100, by either looking up the values in a mathematical reference book, or using a software package that can compute them, or writing your own program to compute them. From this table, compute the entropy, temperature, and heat capacity of this system, using the same methods as in Section 3.3. Plot the heat capacity as a function of temperature, and note that it is approximately linear.

(d) Ramanujan and Hardy (two famous mathematicians) have shown that when q is large, the number of unrestricted partitions of q is given approximately by

p(q)e2q343q

Check the accuracy of this formula for q = 10 and for q = 100. Working in this approximation, calculate the entropy, temperature, and heat capacity of this system. Express the heat. capacity as a series in decreasing powers of kT/, assuming that this ratio is large and keeping the two largest terms. Compare to the numerical results you obtained in part (c). Why is the heat capacity of this system independent of N, unlike that of the three dimensional box of fermions discussed in the text?

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