In this problem you will model helium-3 as a non-interacting Fermi gas. Although He3liquefies at low temperatures, the liquid has an unusually low density and behaves in many ways like a gas because the forces between the atoms are so weak. Helium-3 atoms are spin-1/2 fermions, because of the unpaired neutron in the nucleus.

(a) Pretending that liquid 3He is a non-interacting Fermi gas, calculate the Fermi energy and the Fermi temperature. The molar volume (at low pressures) is 37cm3

(b)Calculate the heat capacity for T<<Tf, and compare to the experimental result CV=(2.8K-1)NkT(in the low-temperature limit). (Don't expect perfect agreement.)

(c)The entropy of solid H3ebelow 1 K is almost entirely due to its multiplicity of nuclear spin alignments. Sketch a graph S vs. T for liquid and solid H3eat low temperature, and estimate the temperature at which the liquid and solid have the same entropy. Discuss the shape of the solid-liquid phase boundary shown in Figure 5.13.

Short Answer

Expert verified

a. The Fermi energy is given byεf=6.8×10-23Jand the Fermi temperature is found to beT=5K.

b. The heat capacity for large Fermi temperature is Cv=1K-1.

c. The temperature at which the liquid and solid have same entropy is given by,T=0.2475k.

Step by step solution

01

Part (a) Step 1: Given information

We have given, the He-3 a non interacting Fermi gas model.

We have to find the Fermi energy and temperature.

02

Simplify

The Fermi energy is given by consider the mass as three proton mass as Helium-3 is,

εf=h28m3NπV23εf=(6.63×10-34J.s)28(3×1.67×10-27kg)3(6.02×1023)π(37×10-6m323εf=6.8×10-23J

Then the Fermi temperature is

T=εfKBT=6.8×10-23J1.38×10-23J/KT=5K

03

Part (b) Step 1: Given information

We have given,

T<<Tf

we have to calculate the heat capacity.

04

Simplify

The heat capacity is given by as in the terms of the given Fermi temperature T is,

Cv=π2NkB2T2εfCvNkBT=(1.34)2(1.38×10-23J/K)2×6.8×10-23JCvNkBT=1.0K-1

This given capacity is greater than found capacity.

05

Part (c) Step 1: Given information

We have given,

T=1K

We have to plot the graph between the entropy S and T.

06

Simplify

The entropy of the liquid ,

S=0TCVTdTS=0T2.8NKTTdTS=2.8NKTK-1

Since,

S=NKlnΩ

By comparing we can say,

T=ln(2)2.8T=0.2475K

here the entropy of liquid will be same for the solids also.

They are connected at one point where the entropy of the system for solid and liquid phase are same as showing in the figure.

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Most popular questions from this chapter

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

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: μν=μν¯. Furthermore, neutrinos and antineutrinos can be produced and annihilated in pairs by the reaction

ν+ν¯2γ

(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?

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 μas 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.

Repeat the previous problem, taking into account the two independent spin states of the electron. Now the system has two "occupied" states, one with the electron in each spin configuration. However, the chemical potential of the electron gas is also slightly different. Show that the ratio of probabilities is the same as before: The spin degeneracy cancels out of the Saha equation.

Starting from equation 7.83, derive a formula for the density of states of a photon gas (or any other gas of ultra relativistic particles having two polarisation states). Sketch this function.

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