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(a) Construct the completely anti symmetric wave function ψ(xA,xB,xC)for three identical fermions, one in the state ψ5, one in the state ψ7,and one in the state ψ17

(b)Construct the completely symmetric wave function ψ(xA,xB,xC)for three identical bosons (i) if all are in state ψ11(ii) if two are in state ψ19and another one is role="math" localid="1658224351718" ψ1c) one in the state ψ5, one in the state ψ7,and one in the stateψ17

Short Answer

Expert verified

(a)The total wave function for fermions is

Ψ(xA,xB,xc)=A36[sin(k5xA)sin(k7xB)sin(k17xC)-sin(k5xA)sin(k17xB)sin(k7xC)]

+A36[sin(k17xA)sin(k7xB)sin(k5xC)-sin(k7xA)sin(k5xB)sin(k17xC)]+A36[sin(k17xA)sin(k5xB)sin(k7xC)-sin(k7xA)sin(k17xB)sin(k5xC)]

(b)The total wave function for bosons are

(i) Ψ(xA,xB,xC)=A36sin(k11xA)sin(k11xB)sin(k11xC)

(ii) Ψ(xA,xB,xC)=23A3[sin(k1xA)sin(k1xB)sin(k19xC)+sin(k1xA)sin(k1xC)sin(k19xB)]+23A3[sin(k1xC)sin(k1xB)sin(k19xA)]

(iii)Ψ(xA,xB,xc)=A366[sin(k5xA)sin(k7xB)sin(k17xC)-sin(k5xA)sin(k17xB)sin(k7xC)]+A36[sin(k17xA)sin(k7xB)sin(k5xC)-sin(k7xA)sin(k5xB)sin(k17xC)]+A36[sin(k17xA)sin(k5xB)sin(k7xC)-sin(k7xA)sin(k17xB)sin(k5xC)]

Step by step solution

01

Define Fermions and bosons

  • Fermions are typically associated with matter, whereas bosons are commonly associated with force carrier particles.
  • However, in today's particle physics, the distinction between the two concepts is blurred.
  • Under extreme conditions, weakly interacting fermions can also exhibit bosonic behavior.
02

Determining the anti-symmetric wave function

a)

If one fermion is in stateψ5, second in state ψ7and third in state ψ17, write down total antisymmetric wave functionψxA,xB,xC. If we assume that fermions are in a square well of with , we can write down a wave function of one particle:

Ψ(x)=Asin(knx)kn=nπA=2a⇒Ψ5=Asin(k5x),Ψ7=Asin(k7x),Ψ17=Asin(k17x)k5=5πa,k7=7πa,k17=17πa

ψxA,xB,xC=16ψAxAψbxBψcxC-ψaxAψcxBψbxC-ψcxAψbxBψaxC+=16-ψbxAψbxBψcxC+ψcxAψaxBψbxC+ψbxAψcxBψaxC

Where Ψa=Ψ5,Ψb=Ψ7,Ψc=Ψ17

The total wave function for fermions is

ψxA,xB,xC=A6sinkAxAsink7xBsink17xC-sink5xAsink17xBsink7xC+A36sink17xAsink7xBsink5xC-sink7xAsink5xBsink17xC+A36sink17xAsink5xBsink7xC-sink7xAsink17xBsink5xC

03

Determining the symmetric wave function

(b)

For bosons, we use the following formula,

ψxA,xB,xC=16ψaxAψbxBψcxC+ψaxAψcxBψbxC+ψcxAψbxBψaxC+=16-ψbxAψaxBψcxC+ψcxAψaxBψbxC+ψbxAψcxBψaxC

(i) If they all are the same state role="math" localid="1658227599599" ψa=ψb=ψc=ψ11, then we have

Ψ(xA,xB,xC)=A36sin(k11xA)sin(k11xB)sin(k11xC)k11=11πaA=2a

(ii) If two of them are same state ψa=ψb=ψ1and the third one is a different state

ψc=ψ19

ψxA,xB,xC=23A3sink1xAsink1xBsink19xC+sink1xAsink1xCsink19xB+23A33sink1xCsink1xBsink19xA

k19=19Ï€ak1=Ï€a,A=2a

(iii)If all of them are in different states Ψa=Ψ5,Ψb=Ψ7,Ψc=Ψ17then total wave

ψxA,xB,xC=A36sink5xAsink7xBsink17xC-sink5xAsink17xBsink7xC=A36sink17xAsink7xBsink5xC-sink7xAsink5xBsink17xC=A36sink17xAsink5xBsink7xC-sink7xAsink17xBsink5xC

Therefore the total wave function for bosons are

(i)Ψ(xA,xB,xC)=A36sin(k11xA)sin(k11xB)sin(k11xC)

(ii) Ψ(xA,xB,xC)=23A3[sin(k1xA)sin(k1xB)sin(k19xC)+sin(k1xA)sin(k1xC)sin(k19xB)]+

23A3[sin(k1xC)sin(k1xB)sin(k19xA)]

(iii) Ψ(xA,xB,xc)=A36[sin(k5xA)sin(k7xB)sin(k17xC)-sin(k5xA)sin(k17xB)sin(k7xC)]+A36[sin(k17xA)sin(k7xB)sin(k5xC)-sin(k7xA)sin(k5xB)sin(k17xC)]+A36[sin(k17xA)sin(k5xB)sin(k7xC)-sin(k7xA)sin(k17xB)sin(k5xC)]

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Most popular questions from this chapter

Suppose you have three particles, and three distinct one-particle stateΨaX,ΨbX,andΨcxare 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 -ΨaX1,ΨaX2Ψax3would be one possibility, if the particles are distinguishable.)

Suppose you had three particles, one in stateψa(x), one in stateψb(x), and one in stateψc(x). Assuming ψa,ψb, andψc 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 isψa(x1),ψb(x1),ψc(x1) , etc., whese second row isψa(x2),ψb(x2),ψc(x2) , etc., and so on (this device works for any number of particles).

(a) Find the percent error in Stirling’s approximation for z = 10 ?

(b)What is the smallest integer z such that the error is less than 1%?

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?

(a) Figure out the electron configurations (in the notation of Equation

5.33) for the first two rows of the Periodic Table (up to neon), and check your

results against Table 5.1.

1s22s22p2(5.33).

(b) Figure out the corresponding total angular momenta, in the notation of

Equation 5.34, for the first four elements. List all the possibilities for boron,

carbon, and nitrogen.

LJ2S+1 (5.34).

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