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Figure 7.37 shows the heat capacity of a Bose gas as a function of temperature. In this problem you will calculate the shape of this unusual graph.

(a) Write down an expression for the total energy of a gas of Nbosons confined to a volume V, in terms of an integral (analogous to equation 7.122).

(b) For T<Tcyou can set =0. Evaluate the integral numerically in this case, then differentiate the result with respect to Tto obtain the heat capacity. Compare to Figure 7.37.

(c) Explain why the heat capacity must approach 32Nkin the high- Tlimit.

(d) For T>Tcyou can evaluate the integral using the values of calculated in Problem 7.69. Do this to obtain the energy as a function of temperature, then numerically differentiate the result to obtain the heat capacity. Plot the heat capacity, and check that your graph agrees with Figure 7.37.

Figure 7.37. Heat capacity of an ideal Bose gas in a three-dimensional box.

Short Answer

Expert verified

(a) Total energy of gas, U=22mh23/2V03/2e(-)/kBT-1d

(b) The expression for heat capacity was obtained.

(c) The reason for the heat capacity to approach32NKin the high Tlimit.

(d) The graph is plotted.

Step by step solution

01

Step 1. Given information

The energy expression for the gas that satisfy the Bose- Einstein's statistics is

U=nnen-kBT-1

Here,

n= energy of the nthparticle,

kB= Boltzmann's constant,

T= temperature.

The energy of the nthparticle is n=g()where g()is the density of states

02

Step 2. (a) To find the total energy of a gas of N bosons confined to volume V

Substitute the value of g()=nin the equationU=nn(en-kBT-1)

U=0g()en-kBT-1d

Substituting the value of 22mh23/2V=g()

U=22mh23/2V03/2e(-)/kBT-1d

Thus, the total energy of a gas of N bosons confined to a volume V= U=22mh23/2V03/2e(-)/kBT-1d

03

Step 3. 

For T<Tcset =0and x=kBTin the expression U=22mh23/2V03/2e(-)/kBT-1d

U=22mh2VkBT5/20x3/2ex-1dx

We know,

0x3/2ex-1dx=3452

=1.783

so,

U=22mh23/2VkBT5/2(1.783)

Specific heat at constant volume of system=

CV=UTV

=T22mh23/2VkBT5/2(1.783)V

=52(1.783)22mh232VkBT3/2kB

=5.0312mh23/2VkBT3/2kB

Using the expression kBTC=0.527h22mNV2/3

CVNkB=5.0312.612TTC3/2

=1.926TTC3/2

This expression shows the nature of slope in the figure 7.37.

For T=Tc, the constant CVNkBis,

CVNkB=1.926TCTC3/2

=1.926

04

Step 4. 

The system ought to behave like a standard substance gas with 3 degrees of freedom at the upper temperature. By the equipartition theorem, the heat capacity should be32NKB

05

Step 5.

The energy of the system =

U=22mh2VkBT5/20x3/2ex-ct-1dx

=(0.432)NkBTC0x3/2ex-ct-1dx

UNkBTC=(0.432)0x3/2ex-ct-1dx

Att=TTC, the above equation is numerically equal toCVNkB.

06

Step 6.

Given below is the graph between CVNkBandTTC

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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路 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=21030kg, 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鈥 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?

Use the results of this section to estimate the contribution of conduction electrons to the heat capacity of one mole of copper at room temperature. How does this contribution compare to that of lattice vibrations, assuming that these are not frozen out? (The electronic contribution has been measured at low temperatures, and turns out to be about40% more than predicted by the free electron model used here.)

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.

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.

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

(b) 0.01eVless than

(c) equal to

(d) 0.01eVgreater than

(e) 1eVgreater than

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