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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.)

Short Answer

Expert verified

The electrons contribute less than 1% of the total heat capacity at room temperature.

Step by step solution

01

Step 1. Given information

The contribution of conduction electrons to the heat capacity of one mole of copper at room temperature is given as

cve=2Nk2T2F

where,

N=the number of atoms and is equal to Avogadro number of atoms per one mole .

k=Boltzmann constant

T=room Temperature

F=the fermi energy.

02

Step 2. Calculating the value of cve

F=7.05eV{The fermi energy of copper }

role="math" localid="1647886513817" Puttingthevalue6.0221023forN,8.61710-5eV/Kfork,300KforT, and7.05eVforF

CVe=26.02210238.61710-5eV/K2(300K)2(7.05eV)

=9.3891017

=9.3891017eV/K1.610-19J/K

=0.15J/K

So, the contribution of conduction electrons to the heat capacity of one mole of copper at room temperature is0.15J/K.

03

Step 3.  Calculating the value of CVl which is the specific heat due to lattice vibration.

According to Debye theory of lattice vibrations, specific heat is given as

CVl=1245TTD3Nk

TD=Debye temperature.

The above formula is applicable whenT<TD.

Duringthe higher temperature whereTTD, the specific heat is

CVI=3Nk

Puttingthevalue6.0221023forNand8.61710-5eV/Kfork

CV/=36.02210231.38110-23J/K

=25J/K

04

Step 4. Calculating the ratio of the contribution of electrons to the heat capacity of the lattice vibrations at room temperature.

So, the contribution of electrons is very small as compared to the heat capacity of the lattice vibrations at room temperature.

CVeCV1=0.15J/K25J/K

=0.006

<1

CVe<CVI

So, the electrons contribute less than1%of the total heat capacity at room temperature.

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Most popular questions from this chapter

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
    p=NkTV(1NvQ42V),
    again neglecting higher-order terms. Thus, quantum statistics results in a lowering of the pressure of a boson gas, as one might expect.
  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.

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 planet Venus is different from the earth in several respects. First, it is only 70% as far from the sun. Second, its thick clouds reflect 77%of all incident sunlight. Finally, its atmosphere is much more opaque to infrared light.

(a) Calculate the solar constant at the location of Venus, and estimate what the average surface temperature of Venus would be if it had no atmosphere and did not reflect any sunlight.

(b) Estimate the surface temperature again, taking the reflectivity of the clouds into account.

(c) The opaqueness of Venus's atmosphere at infrared wavelengths is roughly 70times that of earth's atmosphere. You can therefore model the atmosphere of Venus as 70successive "blankets" of the type considered in the text, with each blanket at a different equilibrium temperature. Use this model to estimate the surface temperature of Venus. (Hint: The temperature of the top layer is what you found in part (b). The next layer down is warmer by a factor of 21/4. The next layer down is warmer by a smaller factor. Keep working your way down until you see the pattern.)

At the surface of the sun, the temperature is approximately 5800 K.

(a) How much energy is contained in the electromagnetic radiation filling a cubic meter of space at the sun's surface?

(b) Sketch the spectrum of this radiation as a function of photon energy. Mark the region of the spectrum that corresponds to visible wavelengths, between 400 nm and 700 nm.

(c) What fraction of the energy is in the visible portion of the spectrum? (Hint: Do the integral numerically.)

The tungsten filament of an incandescent light bulb has a temperature of approximately 3000K. The emissivity of tungsten is approximately 13, and you may assume that it is independent of wavelength.

(a) If the bulb gives off a total of 100watts, what is the surface area of its filament in square millimetres?

(b) At what value of the photon energy does the peak in the bulb's spectrum occur? What is the wavelength corresponding to this photon energy?

(c) Sketch (or use a computer to plot) the spectrum of light given off by the filament. Indicate the region on the graph that corresponds to visible wavelengths, between400and700nm.

(d) Calculate the fraction of the bulb's energy that comes out as visible light. (Do the integral numerically on a calculator or computer.) Check your result qualitatively from the graph of part (c).

( e) To increase the efficiency of an incandescent bulb, would you want to raise or lower the temperature? (Some incandescent bulbs do attain slightly higher efficiency by using a different temperature.)

(f) Estimate the maximum possible efficiency (i.e., fraction of energy in the visible spectrum) of an incandescent bulb, and the corresponding filament temperature. Neglect the fact that tungsten melts at 3695K.

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