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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.

Short Answer

Expert verified

a. The required diagram is given below.

b. The occupancy of each energy level is 191181141121111111100....

c. The value of and Tis nBE=1ee2.2-1.

d. The temperature at q=6from graph iskT=2.35.

Step by step solution

01

Part (a) step 1: Given Information

We need to draw the diagram representing all allowed system states fromq=0up toq=6Instead of using dots.

02

Part (a) step 2:Simplifly

Suppose we have a spin-0bosontrapped in a region where the energy level is evenly spaced, ,the representation of the states from zero energy units q=0to six energy unit q=6is shown unit q=0is shown in the following figure, for q=1there is one state, for q=1there is one state, for q=2 there are two states, for q=3there are three states, for q=4there is five states, for q=5there are seven states and finally for q=6there are eleven states.

03

Part (b) step 1: Given Information

We need to draw a graph of the occupancy as a function of the energy at each level.

04

Part (b) step 2: Simplify

To find the occupancy of each level, we add the number in each level and divide it over 11 states, in the lowest level the sum is 19, in the second-lowest level the sum is 8, in the third-lowest the sum is 4, in the fourth-lowest level the sum is 2, in the fifth-lowest level the sum is1, in the sixth-lowest level the sum is 1,and the sum of the seventh level is zero, so the occupancies are:

191181141121111111100....

the energy of the level equals the spacing between the levels multiplied by the order of the level, so when we plot a graph between the dimensionless energy and the probability, we draw this between and , the graph will looks like this

05

Part (c) step 1: Given Information

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

06

Part (c) step 2: Simplify

For Bose Einstein distribution, the chemical potential equals the energy level when the occupancy goes to infinity, from the graph we see that the occupancy goes to zero at =0,so the chemical potential is zero.Bose-Einstein distribution is given by:

role="math" localid="1649939548278" nBE=1e-kT-1

set =0then,

nBE=1eekT-1

I got a good match when kT=2.2, therefore the Bose-Einstein distribution will be

nBE=1ee2.2-1

I plot this function and the points on the same graph,

07

Part (d) step 1:Given Information 

We need to draw draw a graph of entropy vs energy and estimate the temperature atq=6 from this graph.

08

Part (d) step 2: Simplify

The entropy equals Boltzmann constant multiplies by the natural logarithm of the multiplicity, that is:

Sk=ln

the multiplicities that correspond each energy units are shown in the following table:

qsk010110220.693331.098451.609571.9466112.397

a plot between qandSklooks like this:

09

Part (d) step 3: Calculation

The slope of the graph is :

1Skq=2.397-0.6936-2=0.426

but,

q=Uq=U

thus,

SkU=0.426

the temperature equals the difference in the energy Uover the difference in the entropy that is

T=US

thus,

k1T=0.426

kT=2.35

and which is a rough agreement with the result of part (c).

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Most popular questions from this chapter

Consider a free Fermi gas in two dimensions, confined to a square area A=L2

(a) Find the Fermi energy (in terms of Nand A), and show that the average energy of the particles is F2.

(b) Derive a formula for the density of states. You should find that it is a constant, independent of .

(c) Explain how the chemical potential of this system should behave as a function of temperature, both when role="math" localid="1650186338941" kTFand when Tis much higher.

(d) Because gis a constant for this system, it is possible to carry out the integral 7.53 for the number of particles analytically. Do so, and solve for as a function of N. Show that the resulting formula has the expected qualitative behavior.

(e) Show that in the high-temperature limit, kTF, the chemical potential of this system is the same as that of an ordinary ideal gas.

Consider a gas of noninteracting spin-0 bosons at high temperatures, when TTc. (Note that 鈥渉igh鈥 in this sense can still mean below 1 K.)

  1. Show that, in this limit, the Bose-Einstein function can be written approximately as
    nBE=e()/kT[1+e/kT+].
  2. Keeping only the terms shown above, plug this result into equation 7.122 to derive the first quantum correction to the chemical potential for gas of bosons.
  3. Use the properties of the grand free energy (Problems 5.23 and 7.7) to show that the pressure of any system is given by In P=(kT/V), where Zis the grand partition function. Argue that, for gas of noninteracting particles, In Zcan be computed as the sum over all modes (or single-particle states) of In Zi, where Zi; is the grand partition function for the ithmode.
  4. Continuing with the result of part (c), write the sum over modes as an integral over energy, using the density of states. Evaluate this integral explicitly for gas of noninteracting bosons in the high-temperature limit, using the result of part (b) for the chemical potential and expanding the logarithm as appropriate. When the smoke clears, you should find
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  5. Write the result of part (d) in the form of the virial expansion introduced in Problem 1.17, and read off the second virial coefficient, B(T). Plot the predicted B(T)for a hypothetical gas of noninteracting helium-4 atoms.
  6. Repeat this entire problem for gas of spin-1/2 fermions. (Very few modifications are necessary.) Discuss the results, and plot the predicted virial coefficient for a hypothetical gas of noninteracting helium-3 atoms.

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

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(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?

(a) Estimate (roughly) the total power radiated by your body, neglecting any energy that is returned by your clothes and environment. (Whatever the color of your skin, its emissivity at infrared wavelengths is quite close to 1; almost any nonmetal is a near-perfect blackbody at these wavelengths.)

(b) Compare the total energy radiated by your body in one day (expressed in kilocalories) to the energy in the food you cat. Why is there such a large discrepancy?

(c) The sun has a mass of 21030kgand radiates energy at a rate of 3.91026watts. Which puts out more power per units mass-the sun or your body?

Imagine that there exists a third type of particle, which can share a single-particle state with one other particle of the same type but no more. Thus the number of these particles in any state can be 0,1 or 2 . Derive the distribution function for the average occupancy of a state by particles of this type, and plot the occupancy as a function of the state's energy, for several different temperatures.

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