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Show that when a system is in thermal and diffusive equilibrium with a reservoir, the average number of particles in the system is

N—=kTZ∂Z∂μ

where the partial derivative is taken at fixed temperature and volume. Show also that the mean square number of particles is

N2¯=(kT)2Z∂2Z∂μ2

Use these results to show that the standard deviation of Nis

σN=kT∂N—/∂μ,

in analogy with Problem6.18Finally, apply this formula to an ideal gas, to obtain a simple expression forσNin terms ofN¯Discuss your result briefly.

Short Answer

Expert verified

The simple expression forσN in terms ofN¯isσN=kT∂N—∂μ.

Step by step solution

01

Given Information 

We have to given the average number of particles in the system isN—=kTZ∂Z∂μ, the mean square number of particles is N2¯=(kT)2Z∂2Z∂μ2and the standard deviation of NisσN=kT∂N—/∂μ.

02

Simplify

The grand partition function equals the sum over the Gibbs factors, that is:

Z=∑se−Es−μNs/kT

take the partial derivative of the partition function with respect to , so :

∂Z∂μ=1kT∑sNse−Es−μNs/kT∑sNse−Es−μNs/kT=kT∂Z∂μ

dividing both sides by the grand partition function to get:

1Z∑sNse−Es−μNs/kT=kTZ∂Z∂μ

the LHS is just the average N, so:

localid="1650885600621" N—=kTZ∂Z∂μ ...(1)

take the partial derivative again for the grand partition function with respect toμ, to get:

localid="1650885614351" ∂2Z∂μ2=1k2T2∑s(Ns)2e−Es−μNs/kT∑s(Ns)2e−Es−μNs/kT=k2T2∂2Z∂μ2

03

Calculation

Dividing both sides by the grand partition function to get:

1Z∑s(Ns)2e−Es−μNs/kT=k2T2Z∂2Z∂μ2

the LHS is just the average N2, therefore:

localid="1650885704869" N2—=k2T2Z∂2Z∂μ2 ...(2)

take the partial derivative for the average number of particles with respect to μto get:

localid="1650885695468" role="math" ∂N—∂μ=∂∂μ1Z∑sNse−Es−μNs/kT∂N—∂μ=−1Z2∂Z∂μ∑sNse−Es−μNs/kT+1ZkT∑s(Ns)2e−Es−μNs/kT

substitute from (1) and (2) to get:

∂N—∂μ=−N—kTN—+N2—kT∂N—∂μ=−N—2kT+N2—kTkT∂N—∂μ=N2—−N—2

the standard deviation is defined as:

σN2=N2—−N—2

combine this equation with the previous one to get:

σN2=kT∂N—∂μσN=kT∂N—∂μ

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Most popular questions from this chapter

In Section 6.5 I derived the useful relation F=-kTln(Z)between the Helmholtz free energy and the ordinary partition function. Use analogous argument to prove that ϕ=-kT×ln(Z^), where Z^ is the grand partition function and ϕis the grand free energy introduced in Problem 5.23.

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)

Use the formula P=-(∂U/∂V)S,N to show that the pressure of a photon gas is 1/3 times the energy density (U/V). Compute the pressure exerted by the radiation inside a kiln at 1500 K, and compare to the ordinary gas pressure exerted by the air. Then compute the pressure of the radiation at the centre of the sun, where the temperature is 15 million K. Compare to the gas pressure of the ionised hydrogen, whose density is approximately 105 kg/m3.

The planet Venus is different from the earth in several respects. First, it is only 70% as far from the sun. Second, its thick clouds reflect 77%of all incident sunlight. Finally, its atmosphere is much more opaque to infrared light.

(a) Calculate the solar constant at the location of Venus, and estimate what the average surface temperature of Venus would be if it had no atmosphere and did not reflect any sunlight.

(b) Estimate the surface temperature again, taking the reflectivity of the clouds into account.

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Suppose that the concentration of infrared-absorbing gases in earth's atmosphere were to double, effectively creating a second "blanket" to warm the surface. Estimate the equilibrium surface temperature of the earth that would result from this catastrophe. (Hint: First show that the lower atmospheric blanket is warmer than the upper one by a factor of 21/4. The surface is warmer than the lower blanket by a smaller factor.)

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