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

Short Answer

Expert verified

The final answer, equation 7.68isU35NF+24NF(kT2).

Step by step solution

01

Given information

We have been given that the energy integral 7.54isU=0g()nFD()d.

The Equation 7.67, U=35N52F32+328N(kT)2F+.....and equation 7.68, U=35NF+24N(kT)2F+.....are given.

We need to Carry out the Sommerfeld expansion for the energy integral 7.54to obtain equation 7.67. Then we have to plug in the expansion for to obtain the final answer, equation 7.68.

02

Simplify

The given total energy integral 7.54is

localid="1650054588139" U=0g()nFD()d

localid="1650054613027" U=g0032nFD()d

Integrating by parts, we get:

U=25g053nFD|0-25g0052nFDd (Let this equation be (1))

If we substitute =0, the integral will become zero(0)due to the dependence of the term on 53and the first term vanishes. If we substitute with , the exponential term in the denominator will grow faster than 52.

So the equation (1) reduces to :

U=25g0052nFDd (Let this equation be (2))

We know that nFD=1e(-)kT+1

By Taking derivative with respect to , we get

nFD=1e(-)kT+1

On simplifying,

we getnFD=-1kTe(-)kT(e(-)kT+1)2 (Let this equation be (3))

Let (-)kT=x, the equation (3) becomes :

dx=dkT

Substitute dx,xand nFDin equation (2), we get

U=25g00521kTex(ex+1)2kTdx

U=25g00e52ex(ex+1)2dx (Let this equation be (4))

03

Finding the values of integrals.

As we need to change the integration boundaries also, so :

x0x-kT

As kT, so we can put the lower limit of integral in equation (4) as -,

The integral in equation (4) becomes :

U=25g0-52ex(ex+1)2dx (Let this equation be (5))

Now expand the term 52using Taylor series about ,

52=52+52(-)32+158(-)212+...

Substitute -=kTx,

52=52+52(kTx)32+158(kTx)212+...

Substitute the value of 52in equation (5), we get three integrals say I1,I2,I3,we get:

U=25g0(I1+I2+I3) (Let this equation be (6))

where,

I1=52-ex(ex+1)2dx

I2=52kT32-xex(ex+1)2dx

I3=158(kT)212-x2ex(ex+1)2dx

Simplifying three integrals I1,I2,I3, we get :

I1=52

The second integral I2is odd integral, the integration of integral is from -to , so the integral I2is directly zero .

I2=0

I3=158(kT)21223=528(kT)212

04

Substituting the values of integrals 

By Substituting the values of the three integrals I1,I2,I3in equation (6), we get

U25g052+528(kT)212U25g052+g024(kT)212

Substitute g0=32NF32, we get:

U35NF3252+NF32328(kT)212

Set =Fin second term, we get

U35NF3252+NF328(kT)2 (Let this equation be (7))

The equation (7.66) is given by:

52=F521-212kTF252

By expanding the terms in the brackets, we get:

52=F521-5224kTF2

Substitute the value of 52in equation (7), we get:

U35NF32F521-5224kTF2+NF328(kT)2

U35NF1-5224kTF2+NF328(kT)2

U35NF-18N2FkTF2+NF328(kT)2

U35NF-NF28(kT)2+NF328(kT)2

U35NF+NF2F24(kT)2

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Most popular questions from this chapter

For a system of bosons at room temperature, compute the average occupancy of a single-particle state and the probability of the state containing 0,1,2,3bosons, if the energy of the state is

(a) 0.001eVgreater than

(b) 0.01eVgreater than

(c) 0.1eVgreater than

(d) 1eVgreater than

The argument given above for why CvTdoes not depend on the details of the energy levels available to the fermions, so it should also apply to the model considered in Problem 7.16: a gas of fermions trapped in such a way that the energy levels are evenly spaced and non-degenerate.

(a) Show that, in this model, the number of possible system states for a given value of q is equal to the number of distinct ways of writing q as a sum of positive integers. (For example, there are three system states for q = 3, corresponding to the sums 3, 2 + 1, and 1 + 1 + 1. Note that 2 + 1 and 1 + 2 are not counted separately.) This combinatorial function is called the number of unrestricted partitions of q, denoted p(q). For example, p(3) = 3.

(b) By enumerating the partitions explicitly, compute p(7) and p(8).

(c) Make a table of p(q) for values of q up to 100, by either looking up the values in a mathematical reference book, or using a software package that can compute them, or writing your own program to compute them. From this table, compute the entropy, temperature, and heat capacity of this system, using the same methods as in Section 3.3. Plot the heat capacity as a function of temperature, and note that it is approximately linear.

(d) Ramanujan and Hardy (two famous mathematicians) have shown that when q is large, the number of unrestricted partitions of q is given approximately by

p(q)e2q343q

Check the accuracy of this formula for q = 10 and for q = 100. Working in this approximation, calculate the entropy, temperature, and heat capacity of this system. Express the heat. capacity as a series in decreasing powers of kT/, assuming that this ratio is large and keeping the two largest terms. Compare to the numerical results you obtained in part (c). Why is the heat capacity of this system independent of N, unlike that of the three dimensional box of fermions discussed in the text?

A black hole is a blackbody if ever there was one, so it should emit blackbody radiation, called Hawking radiation. A black hole of mass M has a total energy of Mc2, a surface area of 16G2M2/c4, and a temperature ofhc3/162kGM(as shown in Problem 3.7).

(a) Estimate the typical wavelength of the Hawking radiation emitted by a one-solar-mass (2 x 1030 kg) black hole. Compare your answer to the size of the black hole.

(b) Calculate the total power radiated by a one-solar-mass black hole.

(c) Imagine a black hole in empty space, where it emits radiation but absorbs nothing. As it loses energy, its mass must decrease; one could say it "evaporates." Derive a differential equation for the mass as a function of time, and solve this equation to obtain an expression for the lifetime of a black hole in terms of its initial mass.

(d) Calculate the lifetime of a one-solar-mass black hole, and compare to the estimated age of the known universe (1010 years).

(e) Suppose that a black hole that was created early in the history of the universe finishes evaporating today. What was its initial mass? In what part of the electromagnetic spectrum would most of its radiation have been emitted?

Starting from equation 7.83, derive a formula for the density of states of a photon gas (or any other gas of ultra relativistic particles having two polarisation states). Sketch this function.

In Problem 7.28you found the density of states and the chemical potential for a two-dimensional Fermi gas. Calculate the heat capacity of this gas in the limit role="math" localid="1650099524353" kTF路 Also show that the heat capacity has the expected behavior when kTF. Sketch the heat capacity as a function of temperature.

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