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2. Consider a classical particle moving in a one-dimensional potential well u(x), as shown The particle is in thermal equilibrium with a reservoir at temperature T, so the probabilities of its various states are determined by Boltzmann statistics.

{a) Show that the average position of the particle is given by

where each integral is over the entire xaxis.

A one-dimensional potential well. The higher the temperature, the farther the particle will stray from the equilibrium point.

(b) If the temperature is reasonably low (but still high enough for classical mechanics to apply), the particle will spend most of its time near the bottom of the potential well. In that case we can expand u(x)in a Taylor series about the equilibrium point x0: u(x)=ux0+x-x0dudxx0+12x-x02d2udx2x0

+13!x-x03d3udx3x0+⋯

Show that the linear term must be zero, and that truncating the series after the quadratic term results in the trivial prediction x=x0.

(c) If we keep the cubic term in the Taylor series as well, the integrals in the formula for xbecome difficult. To simplify them, assume that the cubic term is small, so its exponential can be expanded in a Taylor series (leaving the quadratic term in the exponent). Keeping only the smallest temperature-dependent term, show that in this limit x differs from zo by a term proportional to kT. Express the coefficient of this term in terms of the coefficients of the Taylor series foru(x)

(d) The interaction of noble gas atoms can be modeled using the Lennard Jones potential,

u(x)=u0x0x12-2x0x6

Sketch this function, and show that the minimum of the potential well is at x=x0, with depth u0. For argon, x0=3.9Aand u0=0.010eV. Expand the Lennard-Jones potential in a Taylor series about the equilibrium point, and use the result of part ( c) to predict the linear thermal expansion coefficient of a noble gas crystal in terms of u0. Evaluate the result numerically for argon, and compare to the measured value

α=0.0007K-1(at80K)

Short Answer

Expert verified

For argon factor will be doubled.

Step by step solution

01

part(a) Step 1:Given information

Let the particle be associated with position

02

part(a) Step 2: Simplify

x¯=∑xxP(x)=∑xxe-βu(x)Z

03

part(b) Step 1:Given information

The linear tem in the expansion is zero

04

part(b) Step 2: Simplify

∫xe-β∣ux0+ax-x02dx=e-βux0∫xe-βax-x02dx=e-βux0∫y+x0e-βay2dy

∫e-βux0+ax-x02dx=e-βux0∫e-βax-x02dx=e-βux0∫e-βay2dy,

05

part(c) Step 1:Given information

we use Boltzman factor

06

part(c) Step 2: Simplify

x¯=e-βux0∫y+x0e-βay21-βby3dye-βux0∫e-βay21-βby3dy=∫x0-βby4e-βay2dy∫e-βay2dy

x¯=x0-βb3/4β2a2π/βaπ/βa=x0-34bβa2=x0-34ba2kT.

07

part(d) Step 1:Given information

Lennard-Jones is positive

08

part(d) Step 2: Simplify

d3udx3=u0(-12)(-13)(-14)x012x-15-2(-6)(-7)(-8)x06x-9

α=-34ba2kx0=-34-252u0x03x0236u02kx0=748ku0=1.26×10-5eV/Ku0.

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Most popular questions from this chapter

At very high temperatures (as in the very early universe), the proton and the neutron can be thought of as two different states of the same particle, called the "nucleon." (The reactions that convert a proton to a neutron or vice versa require the absorption of an electron or a positron or a neutrino, but all of these particles tend to be very abundant at sufficiently high temperatures.) Since the neutron's mass is higher than the proton's by 2.3 x 10-30 kg, its energy is higher by this amount times c2. Suppose, then, that at some very early time, the nucleons were in thermal equilibrium with the rest of the universe at 1011 K. What fraction of the nucleons at that time were protons, and what fraction were neutrons?

Use a computer to sum the exact rotational partition function numerically, and plot the result as a function ofkT∈. Keep enough terms in the sum to be confident that the series has converged. Show that the approximation in equation 6.31 is a bit low, and estimate by how much. Explain the discrepancy

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Some advances textbooks define entropy by the formula

S=-k∑sPslnPs

where the sum runs over all microstates accessible to the system and Psis the probability of the system being in microstate s.

(a) For an isolated system, role="math" localid="1647056883940" Ps=1Ωfor all accessible states s. Show that in this case the preceding formula reduces to our familiar definition of entropy.

(b) For a system in thermal equilibrium with a reservoir at temperatureT,role="math" localid="1647057328146" Ps=e-EskTZ. Show that in this case as well, the preceding formula agrees with what we already know about entropy.

The most common measure of the fluctuations of a set of numbers away from the average is the standard deviation, defined as follows.

(a) For each atom in the five-atom toy model of Figure 6.5, compute the deviation of the energy from the average energy, that is, Ei-E¯,fori=1to5. Call these deviations ΔEi.

(b) Compute the average of the squares of the five deviations, that is, ΔEi2¯. Then compute the square root of this quantity, which is the root-mean- square (rms) deviation, or standard deviation. Call this number σE. Does σEgive a reasonable measure of how far the individual values tend to stray from the average?

(c) Prove in general that

σE2=E2¯-(E¯)2

that is, the standard deviation squared is the average of the squares minus the square of the average. This formula usually gives the easier way of computing a standard deviation.

(d) Check the preceding formula for the five-atom toy model of Figure 6.5.

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