Evaluate the integral in equation N=2π2πmh23/2V0ϵdϵeϵ/kT-1numerically, to confirm the value quoted in the text.

Short Answer

Expert verified

The integral in equationN=2π2πmh23/2V0ϵdϵeϵ/kT-1is evaluated in simpler form.

Step by step solution

01

Step 1. Given information 

The total number of atoms, Nin Bose-Einstein distribution over all the states is given as:

N=2π2πmh232V0εdεeεkT-1

=2π2πmkTh232V0xex-1dx

Where,

h= Planck's constant,

k= Boltzmann's constant,

V= volume of the box,

ε= energy of the atom for higher energy level,

T= temperature,

m= mass of the atom,

x=εkTis a new variable

02

Step 2. Calculating the integral ∫0∞xdxex-1

Now,

0xdxex-1=0xe-x1-e-xdx

=0x12e-x1-e-x-1

=0x12e-x1+e-x+e-2x+e-3x+dx

=0x12e-x+e-2x+e-3x+e-4x+dx

=0x12k=0e-(k+1)xdx

=k=00x12e-(k+1)xdx

03

Step 3. Solving the integral ∫0∞x12e-(k+1)xdx using the formula  ∫0∞xne-axdx=(n!)a-(n+1)

Therefore,

0x12e-(k+1)x=12!(k+1)-12+1

As we know 12!=Γ12+1, and also Γ12=π

Now,

Γ12+1=12Γ12

=12π

Substituting the value of 12!=12πin the equation 0x12e-(k+1)x=12!(k+1)-12+1we get,

0x12e-(k+1)x=π2(k+1)-32

04

Step 4.  Substituting the value of π2(k+1)-32=∫012x-(k+1)x in the equation

we get,

0xex-1dx=k=0π2(k+1)-32

=π2k=0(k+1)-32

=π21+1232+1332+1432+..

=π2ζ32

05

Step 5. Substitute the value of  ζ32=∑k=1∞1k32=2.612 in the equation 

we get,

0xex-1dx=π2(2.612)

06

Step 6.  Substituting the value of π2(2.612)=∫0∞x12ex-1dx in the equation N=2π2πmkTh232V∫0∞xex-1dx

N=2π2πmkTh232Vπ2(2.612)

=2.6122πmkTh232V

The equation N=2π2πmh23/2V0ϵdϵeϵ/kT-1is evaluated in simpler form.

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Most popular questions from this chapter


Fill in the steps to derive equations 7.112and7.117.

For a brief time in the early universe, the temperature was hot enough to produce large numbers of electron-positron pairs. These pairs then constituted a third type of "background radiation," in addition to the photons and neutrinos (see Figure 7.21). Like neutrinos, electrons and positrons are fermions. Unlike neutrinos, electrons and positrons are known to be massive (ea.ch with the same mass), and each has two independent polarization states. During the time period of interest, the densities of electrons and positrons were approximately equal, so it is a good approximation to set the chemical potentials equal to zero as in Figure 7.21. When the temperature was greater than the electron mass times c2k, the universe was filled with three types of radiation: electrons and positrons (solid arrows); neutrinos (dashed); and photons (wavy). Bathed in this radiation were a few protons and neutrons, roughly one for every billion radiation particles. the previous problem. Recall from special relativity that the energy of a massive particle is ϵ=(pc)2+mc22.

(a) Show that the energy density of electrons and positrons at temperature Tis given by

u(T)=0x2x2+mc2/kT2ex2+mc2/kT2+1dx;whereu(T)=0x2x2+mc2/kT2ex2+mc2/kT2+1dx

(b) Show that u(T)goes to zero when kTmc2, and explain why this is a

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( c) Evaluate u(T)in the limit kTmc2, and compare to the result of the

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(d) Use a computer to calculate and plot u(T)at intermediate temperatures.

(e) Use the method of Problem 7.46, part (d), to show that the free energy

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FV=-16π(kT)4(hc)3f(T);wheref(T)=0x2ln1+e-x2+mc2/kT2dx

Evaluate f(T)in both limits, and use a computer to calculate and plot f(T)at intermediate

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(f) Write the entropy of the electron-positron radiation in terms of the functions

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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?

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