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).

Short Answer

Expert verified

ψ-=ψr1,r2,r3-ψr1,r2,r3-ψr1,r2,r3+ψr2,r3,r1-ψr3,r2,r1+r3,r1,r2-ψr1,r3,r2=0

Step by step solution

01

Definition of Schrodinger equation

The fundamental equation for characterizing quantum mechanical phenomena is the Schrodinger equation. It is a partial differential equation that illustrates how a physical system's wave function changes over time. The electron is a wave in the three-dimensional space surrounding the nucleus.

02

Finding a solution to Schrodinger equation

ψ±=Aψr1,r2,r3,..rz±ψr2,r1,r3,..,rz+ψr2,r3,r1,..,rz+etc.,

Where etc. runs over all permutations of the arguments,r1,r2,..,rz with a + sign for all even permutations (even number of transpositions ri↔rjstarting from r1,r2,..,rzand ± for all odd permutations (+ for bosons, – for fermions).

At the end of the process, normalize the result to determine A. (Typically A=1/Z!, but this may not be right if the starting function is already symmetric under some interchanges.)

If ψ is symmetric in the first two arguments (or any other pair), the anti symmetric combination is zero.

For example, if Z = 3,

ψ-=ψψr1,r2,r3-ψr2,r1,r3+ψr2,r3,r1-r3,r1,r2+ψr3,r1,r2-ψr1,r3,r2=0

(They cancel in pairs).

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 Vaia!

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

Use the method of Lagrange multipliers to find the rectangle of largest area, with sides parallel to the axes that can be inscribed in the ellipse(xa)2+(yb)2=1. What is the maximum area?

Chlorine has two naturally occurring isotopes,CI35and CI37. Show that

the vibrational spectrum of HCIshould consist of closely spaced doublets,

with a splitting given by ∆v=7.51×10-4v, where v is the frequency of the

emitted photon. Hint: Think of it as a harmonic oscillator, with ω=k/μ, where

μis the reduced mass (Equation 5.8 ) and k is presumably the same for both isotopes.

(a) Suppose you put both electrons in a helium atom into the n=2state;

what would the energy of the emitted electron be?

(b) Describe (quantitatively) the spectrum of the helium ion,He+.

(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?

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.

Sign-up for free