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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.

Short Answer

Expert verified

a. The required diagram is given below.

b. The occupancy of each energy level is 191181141121111111100....

c. The value of and Tis nBE=1ee2.2-1.

d. The temperature at q=6from graph iskT=2.35.

Step by step solution

01

Part (a) step 1: Given Information

We need to draw the diagram representing all allowed system states fromq=0up toq=6Instead of using dots.

02

Part (a) step 2:Simplifly

Suppose we have a spin-0bosontrapped in a region where the energy level is evenly spaced, ,the representation of the states from zero energy units q=0to six energy unit q=6is shown unit q=0is shown in the following figure, for q=1there is one state, for q=1there is one state, for q=2 there are two states, for q=3there are three states, for q=4there is five states, for q=5there are seven states and finally for q=6there are eleven states.

03

Part (b) step 1: Given Information

We need to draw a graph of the occupancy as a function of the energy at each level.

04

Part (b) step 2: Simplify

To find the occupancy of each level, we add the number in each level and divide it over 11 states, in the lowest level the sum is 19, in the second-lowest level the sum is 8, in the third-lowest the sum is 4, in the fourth-lowest level the sum is 2, in the fifth-lowest level the sum is1, in the sixth-lowest level the sum is 1,and the sum of the seventh level is zero, so the occupancies are:

191181141121111111100....

the energy of the level equals the spacing between the levels multiplied by the order of the level, so when we plot a graph between the dimensionless energy and the probability, we draw this between and , the graph will looks like this

05

Part (c) step 1: Given Information

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

06

Part (c) step 2: Simplify

For Bose Einstein distribution, the chemical potential equals the energy level when the occupancy goes to infinity, from the graph we see that the occupancy goes to zero at =0,so the chemical potential is zero.Bose-Einstein distribution is given by:

role="math" localid="1649939548278" nBE=1e-kT-1

set =0then,

nBE=1eekT-1

I got a good match when kT=2.2, therefore the Bose-Einstein distribution will be

nBE=1ee2.2-1

I plot this function and the points on the same graph,

07

Part (d) step 1:Given Information 

We need to draw draw a graph of entropy vs energy and estimate the temperature atq=6 from this graph.

08

Part (d) step 2: Simplify

The entropy equals Boltzmann constant multiplies by the natural logarithm of the multiplicity, that is:

Sk=ln

the multiplicities that correspond each energy units are shown in the following table:

qsk010110220.693331.098451.609571.9466112.397

a plot between qandSklooks like this:

09

Part (d) step 3: Calculation

The slope of the graph is :

1Skq=2.397-0.6936-2=0.426

but,

q=Uq=U

thus,

SkU=0.426

the temperature equals the difference in the energy Uover the difference in the entropy that is

T=US

thus,

k1T=0.426

kT=2.35

and which is a rough agreement with the result of part (c).

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Most popular questions from this chapter

The argument given above for why CvTdoes not depend on the details of the energy levels available to the fermions, so it should also apply to the model considered in Problem 7.16: a gas of fermions trapped in such a way that the energy levels are evenly spaced and non-degenerate.

(a) Show that, in this model, the number of possible system states for a given value of q is equal to the number of distinct ways of writing q as a sum of positive integers. (For example, there are three system states for q = 3, corresponding to the sums 3, 2 + 1, and 1 + 1 + 1. Note that 2 + 1 and 1 + 2 are not counted separately.) This combinatorial function is called the number of unrestricted partitions of q, denoted p(q). For example, p(3) = 3.

(b) By enumerating the partitions explicitly, compute p(7) and p(8).

(c) Make a table of p(q) for values of q up to 100, by either looking up the values in a mathematical reference book, or using a software package that can compute them, or writing your own program to compute them. From this table, compute the entropy, temperature, and heat capacity of this system, using the same methods as in Section 3.3. Plot the heat capacity as a function of temperature, and note that it is approximately linear.

(d) Ramanujan and Hardy (two famous mathematicians) have shown that when q is large, the number of unrestricted partitions of q is given approximately by

p(q)e2q343q

Check the accuracy of this formula for q = 10 and for q = 100. Working in this approximation, calculate the entropy, temperature, and heat capacity of this system. Express the heat. capacity as a series in decreasing powers of kT/, assuming that this ratio is large and keeping the two largest terms. Compare to the numerical results you obtained in part (c). Why is the heat capacity of this system independent of N, unlike that of the three dimensional box of fermions discussed in the text?

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.

Calculate the condensate temperature for liquid helium-4, pretending that liquid is a gas of noninteracting atoms. Compare to the observed temperature of the superfluid transition, 2.17K. ( the density of liquid helium-4 is 0.145g/cm3)

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: =. Furthermore, neutrinos and antineutrinos can be produced and annihilated in pairs by the reaction

+2

(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?

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

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