Evaluate the integrand in equation 7.112as a power series in x, keeping terms through x4• Then carry out the integral to find a more accurate expression for the energy in the high-temperature limit. Differentiate this expression to obtain the heat capacity, and use the result to estimate the percent deviation of Cvfrom3NkatT=TDandT=2TD.

Short Answer

Expert verified

The heat capacity isCv=3Nk1120TDT2and the percent deviation of Cvis1.25%.

Step by step solution

01

Given Information 

We need to find calculate the integrand in the equation7.112as a power series inxkeeping terms through x4.

02

Simplify

Equation is given as:

U=9NkT4TD30xmaxx3ex1dx

where,

x=hcsn2LkTxmax=TDT

at low-temperature limit TTD, the value of is very small so we can expand the exponential in the denominator using:

ex1+x+x2/2+x3/6

therefore:

U=9NkT4TD30xmaxx31+x+12x2+16x31U=9NkT4TD30xmaxx3x+12x2+16x3U=9NkT4TD30xmaxx21+12x+16x21

now we can use (1+y)11+y+y2, where y=12x16x2we get :

U=9NkT4TD30xmaxx2112x16x2+12x16x22U=9NkT4TD30xmaxx2112x16x2+14x2+136x4+16x3

neglect the xwith power of 3and4inside the bracket because x is very small ,so:

U=9NkT4TD30xmaxx212x3+112x4

now the function inside the integration is easy to be integrated, so integrate from 0to xmaxto get:

U=9NkT4TD313x318x4+160x50xmaxU=9NkT4TD313xmax318xmax4+160xmax5

but xmax=TTD, so,

U=9NkT4TD313TDT318TDT4+160TDT5U=9NkTD13TTD18+160TDT

the heat capacity at constant volume is the just the partial derivative of the energy with respect to the temperature, that is:

Cv=UT

thus,

localid="1650887002266" Cv=9NkTDT13TTD18+160TDTCv=9NkTD131TD160TDT2Cv=3Nk1120TDT2

03

Calculation

Now calculating the deviation from the asymptotic value 3NkT,atT=TD,

substitute into the above equation we get:

CVT=TD=3Nk1120TDTD2CVT=TD=0.953Nk

so it deviates by 5%AtT=2TD.

CVT=2TD=3Nk1120TD2TD2CVT=2TD=0.98753Nk

so it deviates by1.25%

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Most popular questions from this chapter

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?

An atomic nucleus can be crudely modeled as a gas of nucleons with a number density of 0.18fm-3(where 1fm=10-15m). Because nucleons come in two different types (protons and neutrons), each with spin 1/2, each spatial wavefunction can hold four nucleons. Calculate the Fermi energy of this system, in MeV. Also calculate the Fermi temperature, and comment on the result.

Consider a Bose gas confined in an isotropic harmonic trap, as in the previous problem. For this system, because the energy level structure is much simpler than that of a three-dimensional box, it is feasible to carry out the sum in equation 7.121 numerically, without approximating it as an integral.*

(a) Write equation 7.121 for this system as a sum over energy levels, taking degeneracy into account. Replace Tandμwith the dimensionless variables t=kT/hfandc=μ/hf.

(b) Program a computer to calculate this sum for any given values of tandc. Show that, for N=2000, equation 7.121 is satisfied at t=15provided that c=-10.534. (Hint: You'll need to include approximately the first 200 energy levels in the sum.)

(c) For the same parameters as in part (b), plot the number of particles in each energy level as a function of energy.

(d) Now reduce tto 14 , and adjust the value of cuntil the sum again equals 2000. Plot the number of particles as a function of energy.

(e) Repeat part (d) for t=13,12,11,and10. You should find that the required value of cincreases toward zero but never quite reaches it. Discuss the results in some detail.

Consider a system consisting of a single impurity atom/ion in a semiconductor. Suppose that the impurity atom has one "extra" electron compared to the neighboring atoms, as would a phosphorus atom occupying a lattice site in a silicon crystal. The extra electron is then easily removed, leaving behind a positively charged ion. The ionized electron is called a conduction electron, because it is free to move through the material; the impurity atom is called a donor, because it can "donate" a conduction electron. This system is analogous to the hydrogen atom considered in the previous two problems except that the ionization energy is much less, mainly due to the screening of the ionic charge by the dielectric behavior of the medium.

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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