Physics 48 – Quantum Mechanics...2008/01/28 · Physics 48 – Quantum Mechanics Larry Hunter 120...
Transcript of Physics 48 – Quantum Mechanics...2008/01/28 · Physics 48 – Quantum Mechanics Larry Hunter 120...
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Physics 48 – Quantum Mechanics
Larry Hunter120 Merrill Science CenterX- [email protected]: 101, 104, 108 and 206 Merrill
Office Hours: Monday – 2 PM, Tuesday – 2 PM
Text: Introduction to Quantum Mechanics, Second Edition
David J. Griffiths, (Prentice Hall, 2005)Available at Amherst Books
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What you know?
• Concept of complete orthonormal sets.• Some methods for solving partial
differential equations.• Quantum history – why it was necessary.
– Blackbody radiation – Plank and Leonard– Photo-electric effect – Einstein– Compton Effect– Pair Production
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• Particle Wave Duality (see next slides).• Uncertainty Principle.• Bohr-Rutherford atomic model.• Schrödinger Equation in 1D
t dependent and independent.– Basic intuitions – what solutions should look
like and how they evolve. – Superposition.– Free particle solutions.– QM tunneling and barrier penetration.– Infinite square well.– Finite square well.
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A Reminder about matter waves.
• In Physics 25 you discovered that light must at times be treated as a particle with E = hν and momentum p = E/c = hν/c = h/λ.
• DeBroiglie suggested that matter must have wave-like properties with
λ = h/p.This is seen in experiment.
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Electron Scattering Image of a YIG Xtal
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Molecular beam interference
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Molecular Beam Interference Pattern
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Spin Textures (Interference)
200 225 250 275 300 325 350 375 400
0.0
0.5
1.0
1.5
2.0
Opt
ical
Dep
th
position (μm)
•Anticorrelated•Fringe spacing ~ 25 μm•Confined to overlap region•Not observed if nointerconversion pulse applied
38o
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A quasi-derivation of the S.E.• We demand that
and that
• We assume a non-relativistic limit such that for a free particle.
h//2 pk == λπ
./2 hE== πυω
./22 hmEkmEp =⇒=
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We considered 4 possibilities and assume that the superposition principal must hold (this implies a linear equation – i.e. no terms like Ψ2).
( ) )sin(, kxttx −=Ψ ω
We look for plane wave solutions to describe a free particle
With only this solution the particle can not flicker in and out of existence.
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For a Free particle moving in the +x direction
( ) ( )Ψ x t e i t kx, = − −ω
∂∂
∂∂
ΨΨ Ψ
ΨΨ
ti iE
E it
= − = −
⇒ =
ω / h
h
We can identify the energy operator t
iHδδ
= h
(also called the Hamiltonian, H)
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The Momentum Operator
∂Ψ∂
∂Ψ∂
x ik ip
p ix
= =
⇒ = −
Ψ Ψ
Ψ
h
h
We identify the momentum operator as p ix
= − h∂∂
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∂
∂2
22
2
22Ψ Ψ Ψ Ψ
xk
p mK= − = −
⎛⎝⎜
⎞⎠⎟ =
−h h
( ) ( )Ψ x t e i t kx, = − −ω
⇒ =
−Km x
ΨΨh2 2
22∂∂
We identify the kinetic energy operator Km x
=−h2 2
22∂∂
For a free particle we have Ψ=Ψ HK
With a potential we have the Schrodinger equation as a statement of conservation of energy: Ψ=Ψ+Ψ HUK
The Kinetic Energy Operator
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Ta-Da!The time dependent Schrodinger Equation (TDSE)
( )( ) ( ) ( )
− + =h
h2 2
22mx t
xU x x t i
x tt
∂∂
∂Ψ∂
ΨΨ
,,
,
Note: The Schrödinger equation tells us how to handle conservative forces.Fortunately, nearly all microscopic forces are conservative! In this form we can not handle magnetic forces.
We assume that the potential is not time dependent.
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The absolute value of the square of the wavefunction tells us about the probability of finding the particle at a position x at a time t.
( ) ( )P x t x t, ,= Ψ2
We require that the probability be normalized
( )P x t dx,
Normalization
−∞
∞∫ = 1
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What about our free particle solution?
( ) ( )Ψ x t e i t kx, = − −ω
( ) ( ) ∞===Ψ= ∫ ∫∫∞
∞−
−− dxdxedxtxP kxti 22, ω ?????