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Chapter 40 Introduction to Quantum Physics
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Page 1: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Chapter 40

Introduction to

Quantum Physics

Page 2: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Need for Quantum Physics

Problems remained from classical mechanics that relativity didn’t explain

Attempts to apply the laws of classical physics to explain the behavior of matter on the atomic scale were consistently unsuccessful

Problems included: Blackbody radiation

The electromagnetic radiation emitted by a heated object Photoelectric effect

Emission of electrons by an illuminated metal

Page 3: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Quantum Mechanics Revolution

Between 1900 and 1930, another revolution took place in physics

A new theory called quantum mechanics was successful in explaining the behavior of particles of microscopic size

The first explanation using quantum theory was introduced by Max Planck Many other physicists were involved in other

subsequent developments

Page 4: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Blackbody Radiation

An object at any temperature is known to emit thermal radiation Characteristics depend on the temperature and

surface properties The thermal radiation consists of a continuous

distribution of wavelengths from all portions of the em spectrum

Page 5: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Blackbody Radiation, cont.

At room temperature, the wavelengths of the thermal radiation are mainly in the infrared region

As the surface temperature increases, the wavelength changes It will glow red and eventually white

The basic problem was in understanding the observed distribution in the radiation emitted by a black body Classical physics didn’t adequately describe the observed

distribution

Page 6: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Blackbody Radiation, final

A black body is an ideal system that absorbs all radiation incident on it

The electromagnetic radiation emitted by a black body is called blackbody radiation

Page 7: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Blackbody Approximation

A good approximation of a black body is a small hole leading to the inside of a hollow object

The hole acts as a perfect absorber

The nature of the radiation leaving the cavity through the hole depends only on the temperature of the cavity

Page 8: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Blackbody Experiment Results

The total power of the emitted radiation increases with temperature Stefan’s law (from Chapter 20):

= AeT4

The peak of the wavelength distribution shifts to shorter wavelengths as the temperature increases Wien’s displacement law maxT = 2.898 x 10-3 m.K

Page 9: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Intensity of Blackbody Radiation, Summary

The intensity increases with increasing temperature

The amount of radiation emitted increases with increasing temperature The area under the curve

The peak wavelength decreases with increasing temperature

Page 10: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Active Figure 40.3

Use the active figure to adjust the temperature of the blackbody

Study the emitted radiation

PLAYACTIVE FIGURE

Page 11: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Rayleigh-Jeans Law

An early classical attempt to explain blackbody radiation was the Rayleigh-Jeans law

At long wavelengths, the law matched experimental results fairly well

( ) 4

2I , B∂ ck Të T

ë=

Page 12: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Rayleigh-Jeans Law, cont.

At short wavelengths, there was a major disagreement between the Rayleigh-Jeans law and experiment

This mismatch became known as the ultraviolet catastrophe You would have infinite

energy as the wavelength approaches zero

Page 13: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Max Planck

1858 – 1847 German physicist Introduced the concept

of “quantum of action” In 1918 he was

awarded the Nobel Prize for the discovery of the quantized nature of energy

Page 14: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Planck’s Theory of Blackbody Radiation

In 1900 Planck developed a theory of blackbody radiation that leads to an equation for the intensity of the radiation

This equation is in complete agreement with experimental observations

He assumed the cavity radiation came from atomic oscillations in the cavity walls

Planck made two assumptions about the nature of the oscillators in the cavity walls

Page 15: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Planck’s Assumption, 1

The energy of an oscillator can have only certain discrete values En

En = nhƒ n is a positive integer called the quantum number ƒ is the frequency of oscillation h is Planck’s constant

This says the energy is quantized Each discrete energy value corresponds to a

different quantum state

Page 16: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Planck’s Assumption, 2

The oscillators emit or absorb energy when making a transition from one quantum state to another The entire energy difference between the initial

and final states in the transition is emitted or absorbed as a single quantum of radiation

An oscillator emits or absorbs energy only when it changes quantum states

The energy carried by the quantum of radiation is E = h ƒ

Page 17: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Energy-Level Diagram

An energy-level diagram shows the quantized energy levels and allowed transitions

Energy is on the vertical axis

Horizontal lines represent the allowed energy levels

The double-headed arrows indicate allowed transitions

Page 18: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

More About Planck’s Model

The average energy of a wave is the average energy difference between levels of the oscillator, weighted according to the probability of the wave being emitted

This weighting is described by the Boltzmann distribution law and gives the probability of a state being occupied as being proportional to

where E is the energy of the state BE k Te−

Page 19: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Planck’s Model, Graph

Page 20: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Active Figure 40.7

Use the active figure to investigate the energy levels

Observe the emission of radiation of different wavelengths

PLAYACTIVE FIGURE

Page 21: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Planck’s Wavelength Distribution Function

Planck generated a theoretical expression for the wavelength distribution

h = 6.626 x 10-34 J.s h is a fundamental constant of nature

( ) ( )2

5

2

1I ,

Bhc ëk T

∂ hcë T

ë e=

Page 22: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Planck’s Wavelength Distribution Function, cont.

At long wavelengths, Planck’s equation reduces to the Rayleigh-Jeans expression

At short wavelengths, it predicts an exponential decrease in intensity with decreasing wavelength This is in agreement with experimental results

Page 23: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Photoelectric Effect

The photoelectric effect occurs when light incident on certain metallic surfaces causes electrons to be emitted from those surfaces The emitted electrons are called photoelectrons

Page 24: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Photoelectric Effect Apparatus When the tube is kept in the

dark, the ammeter reads zero

When plate E is illuminated by light having an appropriate wavelength, a current is detected by the ammeter

The current arises from photoelectrons emitted from the negative plate and collected at the positive plate

Page 25: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Active Figure 40.9

Use the active figure to vary frequency or place voltage

Observe the motion of the electrons

PLAYACTIVE FIGURE

Page 26: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Photoelectric Effect, Results At large values of V, the

current reaches a maximum value All the electrons emitted at

E are collected at C The maximum current

increases as the intensity of the incident light increases

When V is negative, the current drops

When V is equal to or more negative than Vs, the current is zero

Page 27: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Active Figure 40.10

Use the active figure to change the voltage range

Observe the current curve for different intensities of radiation

Page 28: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Photoelectric Effect Feature 1

Dependence of photoelectron kinetic energy on light intensity Classical Prediction

Electrons should absorb energy continually from the electromagnetic waves

As the light intensity incident on the metal is increased, the electrons should be ejected with more kinetic energy

Experimental Result The maximum kinetic energy is independent of light

intensity The maximum kinetic energy is proportional to the stopping

potential (Vs)

Page 29: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Photoelectric Effect Feature 2

Time interval between incidence of light and ejection of photoelectrons Classical Prediction

At low light intensities, a measurable time interval should pass between the instant the light is turned on and the time an electron is ejected from the metal

This time interval is required for the electron to absorb the incident radiation before it acquires enough energy to escape from the metal

Experimental Result Electrons are emitted almost instantaneously, even at very

low light intensities

Page 30: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Photoelectric Effect Feature 3

Dependence of ejection of electrons on light frequency Classical Prediction

Electrons should be ejected at any frequency as long as the light intensity is high enough

Experimental Result No electrons are emitted if the incident light falls below

some cutoff frequency, ƒc

The cutoff frequency is characteristic of the material being illuminated

No electrons are ejected below the cutoff frequency regardless of intensity

Page 31: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Photoelectric Effect Feature 4

Dependence of photoelectron kinetic energy on light frequency Classical Prediction

There should be no relationship between the frequency of the light and the electric kinetic energy

The kinetic energy should be related to the intensity of the light

Experimental Result The maximum kinetic energy of the photoelectrons

increases with increasing light frequency

Page 32: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Photoelectric Effect Features, Summary

The experimental results contradict all four classical predictions

Einstein extended Planck’s concept of quantization to electromagnetic waves

All electromagnetic radiation can be considered a stream of quanta, now called photons

A photon of incident light gives all its energy hƒ to a single electron in the metal

Page 33: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Photoelectric Effect, Work Function

Electrons ejected from the surface of the metal and not making collisions with other metal atoms before escaping possess the maximum kinetic energy Kmax

Kmax = hƒ – φ φ is called the work function The work function represents the minimum

energy with which an electron is bound in the metal

Page 34: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Some Work Function Values

Page 35: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Photon Model Explanation of the Photoelectric Effect

Dependence of photoelectron kinetic energy on light intensity Kmax is independent of light intensity K depends on the light frequency and the work

function Time interval between incidence of light and

ejection of the photoelectron Each photon can have enough energy to eject an

electron immediately

Page 36: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Photon Model Explanation of the Photoelectric Effect, cont.

Dependence of ejection of electrons on light frequency There is a failure to observe photoelectric effect

below a certain cutoff frequency, which indicates the photon must have more energy than the work function in order to eject an electron

Without enough energy, an electron cannot be ejected, regardless of the light intensity

Page 37: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Photon Model Explanation of the Photoelectric Effect, final

Dependence of photoelectron kinetic energy on light frequency Since Kmax = hƒ – φ As the frequency increases, the kinetic energy will

increase Once the energy of the work function is exceeded

There is a linear relationship between the kinetic energy and the frequency

Page 38: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Cutoff Frequency

The lines show the linear relationship between K and ƒ

The slope of each line is h

The x-intercept is the cutoff frequency This is the frequency

below which no photoelectrons are emitted

Page 39: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Cutoff Frequency and Wavelength

The cutoff frequency is related to the work function through ƒc = φ / h

The cutoff frequency corresponds to a cutoff wavelength

Wavelengths greater than c incident on a material having a work function φ do not result in the emission of photoelectrons

ƒcc

c hcë

ö= =

Page 40: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Arthur Holly Compton

1892 – 1962 American physicist Director of the lab at

the University of Chicago

Discovered the Compton Effect

Shared the Nobel Prize in 1927

Page 41: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

The Compton Effect, Introduction

Compton and Debye extended with Einstein’s idea of photon momentum

The two groups of experimenters accumulated evidence of the inadequacy of the classical wave theory

The classical wave theory of light failed to explain the scattering of x-rays from electrons

Page 42: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Compton Effect, Classical Predictions

According to the classical theory, em waves incident on electrons should: Have radiation pressure that should cause the

electrons to accelerate Set the electrons oscillating

There should be a range of frequencies for the scattered electrons

Page 43: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Compton Effect, Observations

Compton’s experiments showed that, at any given angle, only one frequency of radiation is observed

Page 44: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Compton Effect, Explanation

The results could be explained by treating the photons as point-like particles having energy hƒ

Assume the energy and momentum of the isolated system of the colliding photon-electron are conserved

This scattering phenomena is known as the Compton effect

Page 45: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Compton Shift Equation

The graphs show the scattered x-ray for various angles

The shifted peak, λ’ is caused by the scattering of free electrons

This is called the Compton shift equation

( )1' cosoe

hë ë è

m c− = −

Page 46: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Compton Wavelength

The factor h/mec in the equation is called the Compton wavelength and is

The unshifted wavelength, λo, is caused by x-rays scattered from the electrons that are tightly bound to the target atoms

0002 43 nmCe

m c= = .

Page 47: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Photons and Waves Revisited

Some experiments are best explained by the photon model

Some are best explained by the wave model We must accept both models and admit that

the true nature of light is not describable in terms of any single classical model

Also, the particle model and the wave model of light complement each other

Page 48: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Louis de Broglie

1892 – 1987 French physicist Originally studied

history Was awarded the

Nobel Prize in 1929 for his prediction of the wave nature of electrons

Page 49: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Wave Properties of Particles

Louis de Broglie postulated that because photons have both wave and particle characteristics, perhaps all forms of matter have both properties

The de Broglie wavelength of a particle is

h hë

p mu= =

Page 50: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Frequency of a Particle

In an analogy with photons, de Broglie postulated that a particle would also have a frequency associated with it

These equations present the dual nature of matter Particle nature, p and E Wave nature, λ and ƒ

ƒE

h=

Page 51: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Davisson-Germer Experiment

If particles have a wave nature, then under the correct conditions, they should exhibit diffraction effects

Davisson and Germer measured the wavelength of electrons

This provided experimental confirmation of the matter waves proposed by de Broglie

Page 52: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Complementarity

The principle of complementarity states that the wave and particle models of either matter or radiation complement each other

Neither model can be used exclusively to describe matter or radiation adequately

Page 53: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Electron Microscope

The electron microscope relies on the wave characteristics of electrons

The electron microscope has a high resolving power because it has a very short wavelength

Typically, the wavelengths of the electrons are about 100 times shorter than that of visible light

Page 54: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Quantum Particle

The quantum particle is a new model that is a result of the recognition of the dual nature

Entities have both particle and wave characteristics

We must choose one appropriate behavior in order to understand a particular phenomenon

Page 55: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Ideal Particle vs. Ideal Wave

An ideal particle has zero size Therefore, it is localized in space

An ideal wave has a single frequency and is infinitely long Therefore,it is unlocalized in space

A localized entity can be built from infinitely long waves

Page 56: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Particle as a Wave Packet

Multiple waves are superimposed so that one of its crests is at x = 0

The result is that all the waves add constructively at x = 0

There is destructive interference at every point except x = 0

The small region of constructive interference is called a wave packet The wave packet can be identified as a particle

Page 57: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Active Figure 40.19

Use the active figure to choose the number of waves to add together

Observe the resulting wave packet

The wave packet represents a particle

PLAYACTIVE FIGURE

Page 58: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Wave Envelope

The blue line represents the envelope function This envelope can travel through space with a

different speed than the individual waves

Page 59: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Active Figure 40.20

Use the active figure to observe the movement of the waves and of the wave envelope

PLAYACTIVE FIGURE

Page 60: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Speeds Associated with Wave Packet

The phase speed of a wave in a wave packet is given by

This is the rate of advance of a crest on a single wave

The group speed is given by

This is the speed of the wave packet itself

phaseùv k=

gdùv dk=

Page 61: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Speeds, cont.

The group speed can also be expressed in terms of energy and momentum

This indicates that the group speed of the wave packet is identical to the speed of the particle that it is modeled to represent

( )2 1

22 2g

dE d pv p u

dp dp m m

⎛ ⎞= = = =⎜ ⎟

⎝ ⎠

Page 62: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Electron Diffraction, Set-Up

Page 63: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Electron Diffraction, Experiment

Parallel beams of mono-energetic electrons that are incident on a double slit

The slit widths are small compared to the electron wavelength

An electron detector is positioned far from the slits at a distance much greater than the slit separation

Page 64: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Electron Diffraction, cont. If the detector collects

electrons for a long enough time, a typical wave interference pattern is produced

This is distinct evidence that electrons are interfering, a wave-like behavior

The interference pattern becomes clearer as the number of electrons reaching the screen increases

Page 65: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Active Figure 40.22

Use the active figure to observe the development of the interference pattern

Observe the destruction of the pattern when you keep track of which slit an electron goes through

Please replace with active figure 40.22

PLAYACTIVE FIGURE

Page 66: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Electron Diffraction, Equations

A maximum occurs when This is the same equation that was used for light

This shows the dual nature of the electron The electrons are detected as particles at a

localized spot at some instant of time The probability of arrival at that spot is determined

by finding the intensity of two interfering waves

sin d è më=

Page 67: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Electron Diffraction Explained An electron interacts with both slits

simultaneously If an attempt is made to determine

experimentally which slit the electron goes through, the act of measuring destroys the interference pattern It is impossible to determine which slit the electron

goes through In effect, the electron goes through both slits

The wave components of the electron are present at both slits at the same time

Page 68: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Werner Heisenberg

1901 – 1976 German physicist Developed matrix

mechanics Many contributions include:

Uncertainty principle Rec’d Nobel Prize in 1932

Prediction of two forms of molecular hydrogen

Theoretical models of the nucleus

Page 69: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

The Uncertainty Principle, Introduction

In classical mechanics, it is possible, in principle, to make measurements with arbitrarily small uncertainty

Quantum theory predicts that it is fundamentally impossible to make simultaneous measurements of a particle’s position and momentum with infinite accuracy

Page 70: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Heisenberg Uncertainty Principle, Statement

The Heisenberg uncertainty principle states: if a measurement of the position of a particle is made with uncertainty x and a simultaneous measurement of its x component of momentum is made with uncertainty px, the product of the two uncertainties can never be smaller than /2

2xx p ≥h

Page 71: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Heisenberg Uncertainty Principle, Explained

It is physically impossible to measure simultaneously the exact position and exact momentum of a particle

The inescapable uncertainties do not arise from imperfections in practical measuring instruments

The uncertainties arise from the quantum structure of matter

Page 72: Chapter 40 Introduction to Quantum Physics. Need for Quantum Physics Problems remained from classical mechanics that relativity didn’t explain Attempts.

Heisenberg Uncertainty Principle, Another Form

Another form of the uncertainty principle can be expressed in terms of energy and time

This suggests that energy conservation can appear to be violated by an amount E as long as it is only for a short time interval t

2E t ≥

h


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