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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

A white dwarf star (see Figure 7.12) is essentially a degenerate electron gas, with a bunch of nuclei mixed in to balance the charge and to provide the gravitational attraction that holds the star together. In this problem you will derive a relation between the mass and the radius of a white dwarf star, modeling the star as a uniform-density sphere. White dwarf stars tend to be extremely hot by our standards; nevertheless, it is an excellent approximation in this problem to set T=0.

(a) Use dimensional analysis to argue that the gravitational potential energy of a uniform-density sphere (mass M, radius R) must equal

Ugrav=-(constant)GM2R

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(b) Assuming that the star contains one proton and one neutron for each electron, and that the electrons are nonrelativistic, show that the total (kinetic) energy of the degenerate electrons equals

Ukinetic=(0.0086)h2M53memp53R2

Figure 7.12. The double star system Sirius A and B. Sirius A (greatly overexposed in the photo) is the brightest star in our night sky. Its companion, Sirius B, is hotter but very faint, indicating that it must be extremely small-a white dwarf. From the orbital motion of the pair we know that Sirius B has about the same mass as our sun. (UCO /Lick Observatory photo.)

( c) The equilibrium radius of the white dwarf is that which minimizes the total energy Ugravity+Ukinetic· Sketch the total energy as a function of R, and find a formula for the equilibrium radius in terms of the mass. As the mass increases, does the radius increase or decrease? Does this make sense?

( d) Evaluate the equilibrium radius for M=2×1030kg, the mass of the sun. Also evaluate the density. How does the density compare to that of water?

( e) Calculate the Fermi energy and the Fermi temperature, for the case considered in part (d). Discuss whether the approximation T = 0 is valid.

(f) Suppose instead that the electrons in the white dwarf star are highly relativistic. Using the result of the previous problem, show that the total kinetic energy of the electrons is now proportional to 1 / R instead of 1R2• Argue that there is no stable equilibrium radius for such a star.

(g) The transition from the nonrelativistic regime to the ultra relativistic regime occurs approximately where the average kinetic energy of an electron is equal to its rest energy, mc2Is the nonrelativistic approximation valid for a one-solar-mass white dwarf? Above what mass would you expect a white dwarf to become relativistic and hence unstable?

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

(c) The opaqueness of Venus's atmosphere at infrared wavelengths is roughly 70times that of earth's atmosphere. You can therefore model the atmosphere of Venus as 70successive "blankets" of the type considered in the text, with each blanket at a different equilibrium temperature. Use this model to estimate the surface temperature of Venus. (Hint: The temperature of the top layer is what you found in part (b). The next layer down is warmer by a factor of 21/4. The next layer down is warmer by a smaller factor. Keep working your way down until you see the pattern.)

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(d) Combine the results of parts (b) and (c) to find an expression for the chemical potential as a function of temperature.

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