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Evaluate the integral in equation N=22mh23/2V0de/kT-1numerically, to confirm the value quoted in the text.

Short Answer

Expert verified

The integral in equationN=22mh23/2V0de/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=22mh232V0dekT-1

=22mkTh232V0xex-1dx

Where,

h= Planck's constant,

k= Boltzmann's constant,

V= volume of the box,

= energy of the atom for higher energy level,

T= temperature,

m= mass of the atom,

x=kTis 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!=12+1, and also 12=

Now,

12+1=1212

=12

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

0x12e-(k+1)x=2(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=02(k+1)-32

=2k=0(k+1)-32

=21+1232+1332+1432+..

=232

05

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

we get,

0xex-1dx=2(2.612)

06

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

N=22mkTh232V2(2.612)

=2.6122mkTh232V

The equation N=22mh23/2V0de/kT-1is evaluated in simpler form.

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Most popular questions from this chapter

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 as 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.

Problem 7.67. In the first achievement of Bose-Einstein condensation with atomic hydrogen, a gas of approximately 21010atoms was trapped and cooled until its peak density was1.81014atoms/cm3. Calculate the condensation temperature for this system, and compare to the measured value of50K.

In analogy with the previous problem, consider a system of identical spin0bosonstrapped in a region where the energy levels are evenly spaced. Assume that Nis a large number, and again let qbe the number of energy units.

(a) Draw diagrams representing all allowed system states from q=0up to q=6.Instead of using dots as in the previous problem, use numbers to indicate the number of bosons occupying each level.

(b) Compute the occupancy of each energy level, for q=6. Draw a graph of the occupancy as a function of the energy at each level.

(c) Estimate values of and Tthat you would have to plug into the Bose-Einstein distribution to best fit the graph of part(b).

(d) As in part (d) of the previous problem, draw a graph of entropy vs energy and estimate the temperature at q=6from this graph.

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(a) Show that the number of photons in equilibrium in a box of volume V at temperature T is

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The integral cannot be done analytically; either look it up in a table or evaluate it numerically.

(b) How does this result compare to the formula derived in the text for the entropy of a photon gas? (What is the entropy per photon, in terms of k?)

(c) Calculate the number of photons per cubic meter at the following temperatures: 300 K; 1500 K (a typical kiln); 2.73 K (the cosmic background radiation).

The sun is the only star whose size we can easily measure directly; astronomers therefore estimate the sizes of other stars using Stefan's law.

(a) The spectrum of Sirius A, plotted as a function of energy, peaks at a photon energy of2.4eV, while Sirius A is approximately 24times as luminous as the sun. How does the radius of Sirius A compare to the sun's radius?

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(c) The spectrum of the star Betelgeuse, plotted as a function of energy, peaks at a photon energy of 0.8eV, while Betelgeuse is approximately10,000times as luminous as the sun. How does the radius of Betelgeuse compare to the sun's radius? Why is Betelgeuse called a "red supergiant"?

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