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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).

Short Answer

Expert verified

a) The distinguishable particles: ψx1,x2,x3isψax1ψbx2ψcx3

b) The identical bosons

ψ1,ψ2,ψ3,-16ψax1ψbx2ψcx3+ψax1ψbx2ψcx3+ψax1ψbx2ψcx3+16ψax1ψbx2ψcx3+ψax1ψbx2ψcx3+ψax1ψbx2ψcx3

c) The identical fermions

ψ1,ψ2,ψ3,-16ψax1ψbx2ψcx3+ψax1ψbx2ψcx3+ψax1ψbx2ψcx3+16ψax1ψbx2ψcx3+ψax1ψbx2ψcx3+ψax1ψbx2ψcx3

Step by step solution

01

Definition of identical bosons ,identical ferminos and slater determinant

  • "Particles come in two types: the particles that make up matter, known as 'fermions,' and the particles that transport forces, known as 'bosons,' according to Carroll.
  • Fermions take up space, whereas bosons can be stacked on top of one another.
  • A Slater determinant is a formula in quantum mechanics that describes the wave function of a multi-fermionic system.
  • It satisfies anti-symmetry criteria, and thus the Pauli principle, by changing sign when two electrons are exchanged (or other fermions)

02

Determine the Slater determinant

WhenNfermionsarepresent,thewholewavefunctioncanberepresentedas:x2,...,xN)=1N!ψax1ψbx1...ψNx1ψax1ψbx1...ψNx2...ψaxNψbxN...ψNxNTheSlaterdeterminantisthenameforthisformula.

03

Determine the distinguishable particles

(a)

The total wave function for identifiable particles is simply the combination of three wave functions:

ψx1,x2,x3=ψax1ψbx2ψcx3

04

Determine the  identical bosons

(b)

When we permute any two particles, the entire wave function for identical bosons must be symmetric:

ψx1,x2,x3,-16ψax1ψbx2ψcx3+ψax1ψbx2ψcx3+ψax1ψbx2ψcx3+16ψax1ψbx2ψcx3+ψax1ψbx2ψcx3+ψax1ψbx2ψcx3

05

Determine the  identical fermions

(c)

When we permute any two fermions, the whole wave function must be antisymmetric for identical fermions:

ψx1,x2,x3,-16ψax1ψbx2ψcx3+ψax1ψbx2ψcx3+ψax1ψbx2ψcx3+16ψax1ψbx2ψcx3+ψax1ψbx2ψcx3+ψax1ψbx2ψcx3

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Most popular questions from this chapter

(a)Use Equation5.113 to determine the energy density in the wavelength rangedλ. Hint: setρ(ω)=ρ-(λ), and solve forρ(λ)-

(b)Derive the Wien displacement law for the wavelength at which the blackbody energy density is a maximum
λmax=2.90×10-3mKT

You'll need to solve the transcendental equation(5×x)=5e-x, using a calculator (or a computer); get the numerical answer accurate to three significant digits.

Evaluate the integrals (Equation5.108 and 5.109) for the case of identical fermions at absolute zero. Compare your results with equations 5.43 and5.45. (Note for electrons there is an extra factor of 2 in Equations 5.108 and 5.109. to account for the spin degeneracy.)

Typically, the interaction potential depends only on the vectorr=r1-r2between

the two particles. In that case the Schrodinger equation seperates, if we change variables from r1,r2andR=(m1r1+m2r2)I(m1+m2)(the center of mass).

(a)Show that

localid="1655976113066" r1=R+(μ/m1)r,r2=R-(μ/m)r,and1=(μ/m)R+r,2=(μ/m1)R-r,where

localid="1655976264171" μ=m1m2m1+m2(5.15).

is the reduced mass of the system

(b) Show that the (time-independent) Schrödinger equation (5.7) becomes

-h22m112ψ-h22m222ψ+=-h22(m1+m2)R2ψ-h22μr2ψ+V(r)ψ=.(5.7).

(c) Separate the variables, letting ψ(R,r)=ψR(R)ψr(r)Note that ψRsatisfies the

one-particle Schrödinger equation, with the total mass (m1+m2)in place of m, potential zero, and energy ERwhile ψrsatisfies the one-particle Schrödinger equation with the reduced mass in place of m, potential V(r) , and energy localid="1655977092786" Er. The total energy is the sum: E=ER+Er. What this tells us is that the center of mass moves like a free particle, and the relative motion (that is, the motion of particle 2 with respect to particle 1) is the same as if we had a single particle with the reduced mass, subject to the potential V. Exactly the same decomposition occurs in classical mechanics; it reduces the two-body problem to an equivalent one-body problem.

Suppose you had three (noninteracting) particles, in thermal equilibrium in a one-dimensional harmonic oscillator potential, with a total energyE=92hω .

(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).

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=h2k22mVπ2k2dk (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?

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