Imagine that there exists a third type of particle, which can share a single-particle state with one other particle of the same type but no more. Thus the number of these particles in any state can be 0,1 or 2 . Derive the distribution function for the average occupancy of a state by particles of this type, and plot the occupancy as a function of the state's energy, for several different temperatures.

Short Answer

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The distribution function for the average occupancy of a state by given types of particles is derived.

The graph is as follows,

Step by step solution

01

Step 1. Given Information 

We are given a particle that can share a single-particle state with one other particle of the same type but no more and the number of these particles in any state can be 0,1or 2.

02

Step 2. Grand partition function

The grand partition function or Gibbs sum is,

Z=ne-n(ϵ-μ)kT

According to the given problem, the number of particles of third type in any state can be 0,1or 2. That is n can be 0,1or2.

Z=n=02exp-n(ε-μ)kTZ=exp(0)+exp-(ε-μ)kT+exp-2(ε-μ)kTZ=1+exp-(ε-μ)kT+exp-2(ε-μ)kT

03

Step 3. Probability of n- particals

Let x=exp-(ε-μ)kT,

Z=1+x+x2

The probability of state being occupied by n-particles is,

P(n)=1Zexp-n(ε-μ)kT=1ZxnP(n)=xn1+x+x2

04

Step 4. Average occupancy of state by particles 

The average occupancy of state by particles of this type is,

n¯=n=02nP(n)=0·P(0)+1·P(1)+2·P(2)=1·x11+x+x2+2·x21+x+x2n¯=x+2x21+x+x2

So, the distribution function for the number of these particles in any state can be 0,1or 2is,

n=x+2x21+x+x2x=exp-(ε-μ)kT

05

Step 5. Graphing the occupancy as a function of the state's energy 

The graph is as follows,

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Most popular questions from this chapter

In the text I claimed that the universe was filled with ionised gas until its temperature cooled to about 3000 K. To see why, assume that the universe contains only photons and hydrogen atoms, with a constant ratio of 109 photons per hydrogen atom. Calculate and plot the fraction of atoms that were ionised as a function of temperature, for temperatures between 0 and 6000 K. How does the result change if the ratio of photons to atoms is 108 or 1010? (Hint: Write everything in terms of dimensionless variables such as t = kT/I, where I is the ionisation energy of hydrogen.)

Consider any two internal states, s1 and s2, of an atom. Let s2 be the higher-energy state, so that Es2-Es1=ϵ 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=ϵ/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=ϵ/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=8πhf3c3

In Problem 7.28you found the density of states and the chemical potential for a two-dimensional Fermi gas. Calculate the heat capacity of this gas in the limit role="math" localid="1650099524353" kTεF· Also show that the heat capacity has the expected behavior when kTεF. Sketch the heat capacity as a function of temperature.

(a) Estimate (roughly) the total power radiated by your body, neglecting any energy that is returned by your clothes and environment. (Whatever the color of your skin, its emissivity at infrared wavelengths is quite close to 1; almost any nonmetal is a near-perfect blackbody at these wavelengths.)

(b) Compare the total energy radiated by your body in one day (expressed in kilocalories) to the energy in the food you cat. Why is there such a large discrepancy?

(c) The sun has a mass of 2×1030kgand radiates energy at a rate of 3.9×1026watts. Which puts out more power per units mass-the sun or your body?

The Sommerfeld expansion is an expansion in powers of kTεF, which is assumed to be small. In this section I kept all terms through order kTεF2, 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" μand 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.)

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