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The Sommerfeld expansion is an expansion in powers of kTεF, which is assumed to be small. In this section I kept all terms through order kTεF2, omitting higher-order terms. Show at each relevant step that the term proportional to localid="1650117451748" T3is zero, so that the next nonvanishing terms in the expansions forlocalid="1650117470867" μand localid="1650117476821" Uare proportional to localid="1650117458596" T4. (If you enjoy such things, you might try evaluating the localid="1650117464980" T4terms, possibly with the aid of a computer algebra program.)

Short Answer

Expert verified

At each step the term proportional to T3is zero and the next nonvanishing terms in the expansion for μand Uare proportional to T4in the proof of expressionU25g0μ52+5π28(kT)2μ12+7π4384(kT)4μ-32

Step by step solution

01

Given information

We have been given that the Sommerfeld expansion is an expansion in powers of kTεF, which is assumed to be small and we kept all terms through order kTεF2, omitting higher-order terms.

We need to show at each relevant step that the term proportional to role="math" localid="1650117659810" T3is zero, so that the next nonvanishing terms in the expansions forμandU are proportional toT4.

02

Simplify

The total energy given by the integral 7.54is:

U=0εg(ε)n¯FD(ε)dε

U=g00ε32n¯FD(ε)dε

Integrating by parts, we get:

U=25g0ε53n¯FD|0+25g00ε52n¯FDεdε (Let this equation be (1))

If we substitute ε=0, the integral becomes zero due to the dependence of the term on ε53and the first term vanishes.

On simplifying, the equation (1) becomes:

U=25g00ε52n¯FDεdε (Let this equation be (2))

We know that n¯FD=1e(ε-μ)kT+1

Taking derivative with respect to ε, we get:

n¯FDε=1e(ε-μ)kT+1ε

On simplifying, we get:

n¯FDε=1kTe(ε-μ)kTe(ε-μ)kT+12

Let localid="1650119493586" (ε-μ)kT=x, then we can write as :

dx=dεkT

Substitute dx,x,n¯FDεin equation (2), we get:
U=25g00ε521kTex(ex+1)2kTdx

U=25g00ε52ex(ex+1)2dx

03

Changing the limits of integration

We need to change the boundaries of integration, so:

εxε0x-μkT

As kTμ, so we can put -as the lower limit of integral, so the integral will become:

U=25g0-ε52ex(ex+1)2dx (Let this equation be (3))

Now by expanding the term ε52about μusing Taylor series, we get:

ε52=μ52+52(ε-μ)μ32+516(ε-μ)2μ12+5128(ε-μ)3μ-12+158(ε-μ)4μ-32...

Substitute ε-μ=kTx, we get:

ε52=μ52+52(kTx)μ32+158(kTx)2μ12+516(kTx)2μ-12+5128(kTx)2μ-32...

04

Finding the values of integrals 

Substitute the value of ε52in equation (3), we get three integral say I1,I2,I3:

U=25g0(I1+I2+I3+I4+I5) (Let this equation be (4))

where, I1=μ52-ex(ex+1)2dx

I2=52kTμ32-xex(ex+1)2dx

I3=158(kT)2μ12-x2ex(ex+1)2dx

I4=516(kT)3μ-12-x3ex(ex+1)2dx

I5=5128(kT)4μ-32-x4ex(ex+1)2dx

On simplifying I1,I2,I3,I4,I5, we get:

role="math" localid="1650601109788" I1=μ52I2=0I3=5π28(kT)2μ12I4=0I5=7π4384(kT)4μ-32

Substituting I1,I2,I3,I4,I5in equation (4), we get:

U25g0μ52+5π28(kT)2μ12+7π2384(kT)4μ-32

We have proved that the proportional term to T3is zero. We can also evaluate the further terms using computer algebra program, if wanted.

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Most popular questions from this chapter

Carry out the Sommerfeld expansion for the energy integral (7.54), to obtain equation 7.67. Then plug in the expansion for μto obtain the final answer, equation 7.68.

Suppose you have a "box" in which each particle may occupy any of 10single-particle states. For simplicity, assume that each of these states has energy zero.

(a) What is the partition function of this system if the box contains only one particle?

(b) What is the partition function of this system if the box contains two distinguishable particles?

(c) What is the partition function if the box contains two identical bosons?

(d) What is the partition function if the box contains two identical fermions?

(e) What would be the partition function of this system according to equation 7.16?

(f) What is the probability of finding both particles in the same single particle state, for the three cases of distinguishable particles, identical bosom, and identical fermions?

Change variables in equation 7.83 to λ=hc/ϵ and thus derive a formula for the photon spectrum as a function of wavelength. Plot this spectrum, and find a numerical formula for the wavelength where the spectrum peaks, in terms of hc/kT. Explain why the peak does not occur at hc/(2.82kT).

Explain in some detail why the three graphs in Figure 7.28 all intercept the vertical axis in about the same place, whereas their slopes differ considerably.

A star that is too heavy to stabilize as a white dwarf can collapse further to form a neutron star: a star made entirely of neutrons, supported against gravitational collapse by degenerate neutron pressure. Repeat the steps of the previous problem for a neutron star, to determine the following: the mass radius relation; the radius, density, Fermi energy, and Fermi temperature of a one-solar-mass neutron star; and the critical mass above which a neutron star becomes relativistic and hence unstable to further collapse.

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