Sketch the heat capacity of copper as a function of temperature from 0to5K, showing the contributions of lattice vibrations and conduction electrons separately. At what temperature are these two contributions equal?

Short Answer

Expert verified

The temperature at which both the contributions are equal is3.7K

Step by step solution

01

Step 1. Given information 

The total heat capacity at low temperature is equal to the sum of the electronic heat capacity lattice vibrational heat capacity.

C=γT+αT3
02

Step 2. Putting the value of γ and α in above equation we get 

Here,γ=π2NkB22εF,α=12Nπ4kB5TD3andTis the temperature.

At low temperature, the electronic contribution to the heat capacity is directly proportional to the temperature.

Celectronic=γT

The contribution of lattice vibrations to the heat capacity has a cubic dependence on temperature at the lower temperature.

Cvibration=αT3
03

Step 3. Now,  solving for the value of γ and α.

Firstly,rearranging the equationC=γT+αT3forCT.

CT=γ+αT2

Here,αis the slope onCTversusT2plot andγis the intercept.

role="math" localid="1647619231371" The slope of the graph betweenCTversusT2of the Copper is as follows:

α=0.9mJ/K218K2

=5×10-5J/K4

The interceptγfor the graph betweenCTversusT2of the Copper is as follows:

γ=0.7mJ/K2

04

Step 4. Calculating the heat capabilities.

The temperature at which the electronic and the lattice vibration contributions of the heat capacities can be calculated by equating the electronic contribution of the heat capacity to the lattice vibration heat capacity.

Celectronic=Cvibration

role="math" localid="1647619436979" SubstituteγTforCelectronicandαT3forCvibration.

γT=αT3

T2=γα

T=γα

Substitute0.7mJ/K2forγand5×10-5J/K4forα.

T=0.7mJ/K210-3J1mJ5×10-5J/K4

=3.7K

At this temperature, both heat capacities are as follows:

Celectronic=γT

Substitute0.7mJ/K2forγand3.7KforT

Celectronic=0.7mJ/K210-3J1mJ(3.7K)

=0.0026J/K.

05

Step 5. Using the table that shows the data for the temperature and the electronic heat capacity lattice vibrational heat capacity for the copper.

The table we have,

T(in K)Cclectronic=γTCvibation=αT300010.00070.0000520.00140.000430.00210.0013540.00280.003250.00350.00625

06

Step 6. Plotted the graph between CV and temperature for the lattice vibration and electron contributions.

So, the required plot we have is shown below

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Most popular questions from this chapter

Most spin-1/2 fermions, including electrons and helium-3 atoms, have nonzero magnetic moments. A gas of such particles is therefore paramagnetic. Consider, for example, a gas of free electrons, confined inside a three-dimensional box. The z component of the magnetic moment of each electron is ±µa. In the presence of a magnetic field B pointing in the z direction, each "up" state acquires an additional energy of -μBB, while each "down" state acquires an additional energy of +μBB

(a) Explain why you would expect the magnetization of a degenerate electron gas to be substantially less than that of the electronic paramagnets studied in Chapters 3 and 6, for a given number of particles at a given field strength.

(b) Write down a formula for the density of states of this system in the presence of a magnetic field B, and interpret your formula graphically.

(c) The magnetization of this system is μBN-N, where Nr and N1 are the numbers of electrons with up and down magnetic moments, respectively. Find a formula for the magnetization of this system at T=0, in terms of N, µa, B, and the Fermi energy.

(d) Find the first temperature-dependent correction to your answer to part (c), in the limit TTF. You may assume that μBBkT; this implies that the presence of the magnetic field has negligible effect on the chemical potential μ. (To avoid confusing µB with µ, I suggest using an abbreviation such as o for the quantity µaB.)

In the text I claimed that the universe was filled with ionised gas until its temperature cooled to about 3000 K. To see why, assume that the universe contains only photons and hydrogen atoms, with a constant ratio of 109 photons per hydrogen atom. Calculate and plot the fraction of atoms that were ionised as a function of temperature, for temperatures between 0 and 6000 K. How does the result change if the ratio of photons to atoms is 108 or 1010? (Hint: Write everything in terms of dimensionless variables such as t = kT/I, where I is the ionisation energy of hydrogen.)

In a real semiconductor, the density of states at the bottom of the conduction band will differ from the model used in the previous problem by a numerical factor, which can be small or large depending on the material. Let us, therefore, write for the conduction band g(ϵ)=g0cϵ-ϵcwhere g0cis a new normalization constant that differs from g0by some fudge factor. Similarly, write gat the top of the valence band in terms of a new normalization constant g0v.

(a) Explain why, if g0vg0c, the chemical potential will now vary with temperature. When will it increase, and when will it decrease?

(b) Write down an expression for the number of conduction electrons, in terms of T,μ,candg0cSimplify this expression as much as possible, assuming ϵc-μkT.

(c) An empty state in the valence band is called a hole. In analogy to part (b), write down an expression for the number of holes, and simplify it in the limit μ-ϵvkT.

(d) Combine the results of parts (b) and (c) to find an expression for the chemical potential as a function of temperature.

(e) For silicon, g0cg0=1.09andg0vg0=0.44*.Calculate the shift inµ for silicon at room temperature.

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.

It's not obvious from Figure 7.19 how the Planck spectrum changes as a function of temperature. To examine the temperature dependence, make a quantitative plot of the functionu(ϵ) for T = 3000 K and T = 6000 K (both on the same graph). Label the horizontal axis in electron-volts.

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