/*! This file is auto-generated */ .wp-block-button__link{color:#fff;background-color:#32373c;border-radius:9999px;box-shadow:none;text-decoration:none;padding:calc(.667em + 2px) calc(1.333em + 2px);font-size:1.125em}.wp-block-file__button{background:#32373c;color:#fff;text-decoration:none} Q 7.44 Number of photons in a photon ga... [FREE SOLUTION] | 91影视

91影视

Number of photons in a photon gas.

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

N=8VkThc30x2ex-1dx

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).

Short Answer

Expert verified

Hence, the number of photons per cubic metre is

NV300=5.4581014m-3NV1500=6.821016m-3NV2.73=4.11108m-3

Step by step solution

01

Given information

Number of photons in a photon gas.

Number of photons in equilibrium in a box of volume V at temperature T is

N=8VkThc30x2ex-1dx

02

Explanation

Because we have two polarisation modes, the number of photons equals the total of Planck distributions over all modes nx,nyandnz, multiplied by a factor of two, that is:

N=2nxnynznPl()=nx,ny,nznPl()

But, nPl()=1e/kT-1

Consider a cubic box with a volume of V and a side width of L; the photon's permitted energy is:

=hcn2L

Substitute this the above equation:

N=2nx,ny,nz1ehcn/2LkT-1

Now we need to convert the total to an integral in spherical coordinates, which we can do by multiplying it by the spherical integration factor n2sin()which gives us:

N=20/2d0/2sin()d0n2ehcn/2LkT-1dn

So,

N=0n2ehcn/2LkT-1dn

Now, let

x=hcn2LkTdx=hc2LkTdn

Thus,

N=2LkThc30x2ex-1dx

The volume of the box is V=L3

N=8VkThc30x2ex-1dx

Evaluate the integral:

0x2ex-1dx

We get

x=2.4041

03

Explanation

The number of photons is:

N=8(2.404)VkThc3(1)

The entropy is:

S(T)=32545VkThc3k

Hence, entropy per photon is:

SN=32545VkThc3k8(2.404)VkThc3=3.60kSN=3.60k

(c) To find the number of photons per cubic meter at T= 300 K, substitute the values

NV300=8(2.404)1.3810-23J/K(300K)6.62610-34Js3.0108m/s3NV300=5.4581014m-3NV1500=8(2.404)1.3810-23J/K(300K)6.62610-34Js3.0108m/s3NV1500=6.821016m-3NV2.73=8(2.404)1.3810-23J/K(300K)6.62610-34Js3.0108m/s3NV2.73=4.11108m-3

Unlock Step-by-Step Solutions & Ace Your Exams!

  • Full Textbook Solutions

    Get detailed explanations and key concepts

  • Unlimited Al creation

    Al flashcards, explanations, exams and more...

  • Ads-free access

    To over 500 millions flashcards

  • Money-back guarantee

    We refund you if you fail your exam.

Over 30 million students worldwide already upgrade their learning with 91影视!

One App. One Place for Learning.

All the tools & learning materials you need for study success - in one app.

Get started for free

Most popular questions from this chapter

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.

For a system of bosons at room temperature, compute the average occupancy of a single-particle state and the probability of the state containing 0,1,2,3bosons, if the energy of the state is

(a) 0.001eVgreater than

(b) 0.01eVgreater than

(c) 0.1eVgreater than

(d) 1eVgreater than

Consider any two internal states, s1 and s2, of an atom. Let s2 be the higher-energy state, so that Es2-Es1= for some positive constant. If the atom is currently in state s2, then there is a certain probability per unit time for it to spontaneously decay down to state s1, emitting a photon with energy e. This probability per unit time is called the Einstein A coefficient:

A = probability of spontaneous decay per unit time.

On the other hand, if the atom is currently in state s1 and we shine light on it with frequency f=/h, then there is a chance that it will absorb photon, jumping into state s2. The probability for this to occur is proportional not only to the amount of time elapsed but also to the intensity of the light, or more precisely, the energy density of the light per unit frequency, u(f). (This is the function which, when integrated over any frequency interval, gives the energy per unit volume within that frequency interval. For our atomic transition, all that matters is the value of u(f)atf=/h) The probability of absorbing a photon, per unit time per unit intensity, is called the Einstein B coefficient:

B=probability of absorption per unit timeu(f)

Finally, it is also possible for the atom to make a stimulated transition from s2down to s1, again with a probability that is proportional to the intensity of light at frequency f. (Stimulated emission is the fundamental mechanism of the laser: Light Amplification by Stimulated Emission of Radiation.) Thus we define a third coefficient, B, that is analogous to B:

B'=probability of stimulated emission per unit timeu(f)

As Einstein showed in 1917, knowing any one of these three coefficients is as good as knowing them all.

(a) Imagine a collection of many of these atoms, such that N1 of them are in state s1 and N2 are in state s2. Write down a formula for dN1/dt in terms of A, B, B', N1, N2, and u(f).

(b) Einstein's trick is to imagine that these atoms are bathed in thermal radiation, so that u(f) is the Planck spectral function. At equilibrium, N1and N2 should be constant in time, with their ratio given by a simple Boltzmann factor. Show, then, that the coefficients must be related by

B'=BandAB=8hf3c3

For a system of particles at room temperature, how large must -be before the Fermi-Dirac, Bose-Einstein, and Boltzmann distributions agree within 1%? Is this condition ever violated for the gases in our atmosphere? Explain.

The Sommerfeld expansion is an expansion in powers of kTF, which is assumed to be small. In this section I kept all terms through order kTF2, omitting higher-order terms. Show at each relevant step that the term proportional to localid="1650117451748" T3is zero, so that the next nonvanishing terms in the expansions forlocalid="1650117470867" and localid="1650117476821" Uare proportional to localid="1650117458596" T4. (If you enjoy such things, you might try evaluating the localid="1650117464980" T4terms, possibly with the aid of a computer algebra program.)

See all solutions

Recommended explanations on Physics Textbooks

View all explanations

What do you think about this solution?

We value your feedback to improve our textbook solutions.

Study anywhere. Anytime. Across all devices.