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In Section 2.5 I quoted a theorem on the multiplicity of any system with only quadratic degrees of freedom: In the high-temperature limit where the number of units of energy is much larger than the number of degrees of freedom, the multiplicity of any such system is proportional to UNf/2, whereNf is the total number of degrees of freedom. Find an expression for the energy of such a system in terms of its temperature, and comment on the result. How can you tell that this formula forΩ cannot be valid when the total energy is very small?

Short Answer

Expert verified

The required expression isU=f2NkT.

Step by step solution

01

Given

It is given that,

ΩUNf2,

where,

Nfis the total number of degrees of freedom

Expression for multiplicity that is given as:

Ω=VN(2πmU)3N2h3NN!3N2!

And for Einstein solid in the high temperature limit expression for multiplicity is given as:

ΩqeNN

Here, Nis number of oscillator in solid, qis number of energy unit.

02

Calculation

Mathematically, temperature can be defined as:

1T=SU..........(1)

Where,

Sis the change in entropy and Uis the change in the internal energy of the body.

The given system has two quadratic terms in its energy. One is potential energy 12kx2and another one is kinetic energy term 12mv2. Each of this is interpreted as degree of freedom.

So, multiplicity is written as:

localid="1646989414665" ΩUNf2Ω=AUNF2

Here, Ais constant of proportionality.

Now, Entropy is given by

S=klnΩ

Where, kis Boltzmann constant and Ωis multiplicity.

By substituting the value of Ωin the above, we get,

S=klnAUNf2

But we know that,

lnab=bln(a),lnab=ln(a)-ln(b)and lnab=bln(a)

Hence,

S=kln(A)+Nfk2lnU

Now, by substituting this value of Sin the equation (1), we get,

localid="1646990034822" 1T=SU=Ukln(A)+Nfk2lnU1T=Nfk2UT=2UNfk

By rearranging the terms, we get,

U=f2NkT

03

Final answer

Hence, the required expression for the energy of the given system in terms of its temperature isU=f2NkT.

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Most popular questions from this chapter

In Problem 1.55 you used the virial theorem to estimate the heat capacity of a star. Starting with that result, calculate the entropy of a star, first in terms of its average temperature and then in terms of its total energy. Sketch the entropy as a function of energy, and comment on the shape of the graph.

Use a computer to study the entropy, temperature, and heat capacity of an Einstein solid, as follows. Let the solid contain 50 oscillators (initially), and from 0 to 100 units of energy. Make a table, analogous to Table 3.2, in which each row represents a different value for the energy. Use separate columns for the energy, multiplicity, entropy, temperature, and heat capacity. To calculate the temperature, evaluate ΔU/ΔSfor two nearby rows in the table. (Recall that U=qϵfor some constant ϵ.) The heat capacity (ΔU/ΔT)can be computed in a similar way. The first few rows of the table should look something like this:

(In this table I have computed derivatives using a "centered-difference" approximation. For example, the temperature .28is computed as 2/(7.15-0).) Make a graph of entropy vs. energy and a graph of heat capacity vs. temperature. Then change the number of oscillators to 5000 (to "dilute" the system and look at lower temperatures), and again make a graph of heat capacity vs. temperature. Discuss your prediction for the heat capacity, and compare it to the data for lead, aluminum, and diamond shown in Figure 1.14. Estimate the numerical value of εin electron-volts, for each of those real solids.

In the experiment of Purcell and Pound, the maximum magnetic field strength was 0.63Tand the initial temperature was 300K. Pretending that the lithium nuclei have only two possible spin states (in fact they have four), calculate the magnetization per particle, M/N, for this system. Take the constant μto be 5×10-8eV/T. To detect such a tiny magnetization, the experimenters used resonant absorption and emission of radio waves. Calculate the energy that a radio wave photon should have, in order to flip a single nucleus from one magnetic state to the other. What is the wavelength of such a photon?

Use the result of Problem 2.42 to calculate the temperature of a black hole, in terms of its mass M. (The energy is Mc2. ) Evaluate the resulting expression for a one-solar-mass black hole. Also sketch the entropy as a function of energy, and discuss the implications of the shape of the graph.

What partial-derivative relation can you derive from the thermodynamic identity by considering a process that takes place at constant entropy? Does the resulting equation agree with what you already knew? Explain.

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