/*! This file is auto-generated */ .wp-block-button__link{color:#fff;background-color:#32373c;border-radius:9999px;box-shadow:none;text-decoration:none;padding:calc(.667em + 2px) calc(1.333em + 2px);font-size:1.125em}.wp-block-file__button{background:#32373c;color:#fff;text-decoration:none} Q24P Check the equations 5.74, 5.75, ... [FREE SOLUTION] | 91影视

91影视

Check the equations 5.74, 5.75, and 5.77 for the example in section 5.4.1

Short Answer

Expert verified

Using equations for several occupied states to distinguish particles, fermions, and bosons, we calculated several occupied states.

First configurationN11=3others zeroQd=6.13!=1Qf=0Qb=1

Second configurationN5=1,N13=2:others zeroQd=6.11!.12!=3Qf=0Qb=1

Third configurationN1=2,N19=1:others zeroQd=6.11!.12!=3Qf=0Qb=1

Fourth configuration N5=N7=N17others zero Qd=6=3Qf=0Qb=1

Step by step solution

01

Define Fermions and bosons

  • Bosons are frequently connected with force carrier particles, whereas fermions are typically associated with matter.
  • Today's particle physics, however, makes it difficult to distinguish between the two ideas.
  • Under extreme conditions, weakly interacting fermions can also exhibit bosonic behavior.
02

Determining the occupied states using formulae

Need to check if equationsandgive the same result as counting states "by hand" in example in Section 5.4.1. We calculate occupied states for distinguishable particles, fermions and bosons by formulae:

Qd(N1,N2,N3,....)=N!n-1dnNnNn!Qf(N1,N2,N3,....)=n-1dn!Nn!(dn-Nn)!Qb(N1,N2,N3,....)=n-1(Nn+dn-1)!Nn!(dn-1)!

Where is number of particles in the system and is degree of degeneracy of oneparticle state. For all configurations in example and . So we have:

Qd=6n-11Nn!Qf=n-11Nn!(1-Nn)!Qf=n-1NnNn!=1

03

Calculating the occupied states

So, the number of occupied states

First configurationN11=3others zero Qd=6.13!=1Qf=0Qb=1

Second configurationN5=1,N13=2:others zeroQd=6.11!.12!=3Qf=0Qb=1

Third configurationN1=2,N19=1:others zeroQd=6.11!.12!=3Qf=0Qb=1

Fourth configurationN5=N7=N17others zerorole="math" localid="1658218029425" Qd=6=6Qf=0Qb=1

Using equations for number of occupied states for distinguishable particles, fermions and bosons, we calculated number of occupied states for example in Section 5.4.1.

Unlock Step-by-Step Solutions & Ace Your Exams!

  • Full Textbook Solutions

    Get detailed explanations and key concepts

  • Unlimited Al creation

    Al flashcards, explanations, exams and more...

  • Ads-free access

    To over 500 millions flashcards

  • Money-back guarantee

    We refund you if you fail your exam.

Over 30 million students worldwide already upgrade their learning with 91影视!

One App. One Place for Learning.

All the tools & learning materials you need for study success - in one app.

Get started for free

Most popular questions from this chapter

We can extend the theory of a free electron gas (Section 5.3.1) to the relativistic domain by replacing the classical kinetic energy, E=p2/2m,,with the relativistic formula, E=p2c2+m2c4-mc2. Momentum is related to the wave vector in the usual way: p=hk. In particular, in the extreme relativistic limit, Epc=hck.

(a) Replace h2k2n Equation 5.55 by the ultra-relativistic expression, hck, and calculateEtotin this regime.

dE=h2k22mV2k2dk (5.55).

(b) Repeat parts (a) and (b) of Problem 5.35 for the ultra-relativistic electron gas. Notice that in this case there is no stable minimum, regardless of R; if the total energy is positive, degeneracy forces exceed gravitational forces, and the star will expand, whereas if the total is negative, gravitational forces win out, and the star will collapse. Find the critical number of nucleons, Nc , such that gravitational collapse occurs for N>N_{C}is called the Chandrasekhar limit.

(c) At extremely high density, inverse beta decaye-+p+n+v,converts virtually all of the protons and electrons into neutrons (liberating neutrinos, which carry off energy, in the process). Eventually neutron degeneracy pressure stabilizes the collapse, just as electron degeneracy does for the white dwarf (see Problem 5.35). Calculate the radius of a neutron star with the mass of the sun. Also calculate the (neutron) Fermi energy, and compare it to the rest energy of a neutron. Is it reasonable to treat a neutron star non relativistic ally?

Suppose you had three particles, one in statea(x), one in stateb(x), and one in statec(x). Assuming a,b, andc are orthonormal, construct the three-particle states (analogous to Equations 5.15,5.16, and 5.17) representing

(a) distinguishable particles,

(b) identical bosons, and

(c) identical fermions.

Keep in mind that (b) must be completely symmetric, under interchange of any pair of particles, and (c) must be completely antisymmetric, in the same sense. Comment: There's a cute trick for constructing completely antisymmetric wave functions: Form the Slater determinant, whose first row isa(x1),b(x1),c(x1) , etc., whese second row isa(x2),b(x2),c(x2) , etc., and so on (this device works for any number of particles).

Suppose you have three particles, and three distinct one-particle stateaX,bX,andcxare available. How many different three-particle states can be constructed (a) if they are distinguishable particles, (b) if they are identical bosons, (c) if they are identical fermions? (The particles need not be in different states -aX1,aX2ax3would be one possibility, if the particles are distinguishable.)

Calculate the Fermi energy for noninteracting electrons in a two-dimensional infinite square well. Let 蟽 be the number of free electrons per unit area.

(a) Using Equations 5.59 and 5.63, show that the wave function for a particle in the periodic delta-function potential can be written in the form

(X)=C[sinkx+e-ikasina-x]0xa

(b) There is an exception; At the top of a band where z is an integer multiple ofyiels(x)=0 yields .

Find the correct wave function for the case. Note what happens toeach delta function.

See all solutions

Recommended explanations on Physics Textbooks

View all explanations

What do you think about this solution?

We value your feedback to improve our textbook solutions.

Study anywhere. Anytime. Across all devices.