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Imagine two noninteracting particles, each of mass m, in the infinite square well. If one is in the stateψn(Equation 2.28 ), and the other in state ψ1(l≠n), calculate localid="1658214464999" (x1-x2)2, assuming (a) they are distinguishable particles, (b) they are identical bosons, and (c) they are identical fermions.

Short Answer

Expert verified

a) The value of<(x1-x2)2>assuming that they are distinguishable particles is a216-12Ï€21n2+1m2.

b) The value of<(x1-x2)2>assuming that they are identical bosons is a216-12Ï€21n2+1m2-128a2m2n2Ï€4m2-n24

c) The value of<(x1-x2)2>assuming that they are identical fermions is a216-12Ï€21n2+1m2-128a2m2n2Ï€4m2-n24.

Step by step solution

01

Definition of identical bosons and identical fermions

According to Carroll, particles exist in two types: those that makeup matter, known as 'fermions,' and those that convey forces, known as 'bosons.

Bosons can be piled on top of one other, whereas fermions take up space.

02

(a) Determination of <(x1-x2)2> assuming that they are distinguishable particles

For distinguishable particles, use the following formula,

x1-x22=x2a+x2b-2xa(xnb~=a213-12ττ²Ô2+a213-12ττ²Ô2-2×a2×a2=a223-12-12ττ21n2+1m2Evaluatethevalueofx1-x22.x1-x22=a216-12ττ21n2+1m2Thus,thevalueofx1-x22assumingtheyaredistinguishableparticlesisa216-12ττ21n2+1m2.

03

(b) Determination of<x1-x22>assuming that they are the identical Bosons

For the same Bosons, the equation is as follows,

x1-x22B=x2m+x2n-2a,xn~na,xn~m-2a,xn~nm2=x1-x22d-2a,xn~nm2

But it is known that a,xn~nm=-8amnττ2m2-n22. So, that expression is as follows,

a,xn~nm2=a,xn~nm2=a,xn~nma,xn~nmx1-x22B=a216-12ττ21n2+1m2-128a2m2n2ττ4m2-n2Hence,thevalueofx1-x22dconsideringtheyareidenticalbosonsis.a216-12ττ21n2+1m2-128a2m2n2ττ4m2-n24

04

(c) Determination of<x1-x22>assuming that they are the identical fermions

ForFermionsthatareidentical,theequationisasfollows,x1-x2f2=xa2+xb2-2ax,n~aax,n~b+2ax,n~ab2=x1-x2d2+2ax,n~ab2=a216-12ττ21n2+1m2+128a2m2n2ττ4m2-n24Thus,thevalueofx1-x22dwhentheyareidenticalfermionsis.=a216-12ττ21n2+1m2+128a2m2n2ττ4m2-n24

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Most popular questions from this chapter

Suppose you could find a solutionψ(r1,r2,...,rz)to the Schrödinger equation (Equation 5.25), for the Hamiltonian in Equation 5.24. Describe how you would construct from it a completely symmetric function, and a completely anti symmetric function, which also satisfy the Schrödinger equation, with the same energy.

role="math" localid="1658219144812" H^=∑j=1Z-ħ22m∇j2-14πo,0Ze2rj+1214πo,0∑j≠1Ze2rj-rk (5.24).

role="math" localid="1658219153183" H^ψ=E (5.25).

(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

ψ(X)=C[sinkx+e-ikasina-x]0≤x≤a

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

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

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, E≈pc=hck.

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

dE=h2k22mVÏ€2k2dk (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 (noninteracting) particles, in thermal equilibrium in a one-dimensional harmonic oscillator potential, with a total energyE=92hÓ¬ .

(a) If they are distinguishable particles (but all with the same mass), what are the possible occupation-number configurations, and how many distinct (threeparticle) states are there for each one? What is the most probable configuration? If you picked a particle at random and measured its energy, what values might you get, and what is the probability of each one? What is the most probable energy?

(b) Do the same for the case of identical fermions (ignoring spin, as we did in Section 5.4.1).

(c) Do the same for the case of identical bosons (ignoring spin).

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