A. 0.7 ev B. 1.1 ev C. 1.4 ev D. 1.8 ev E. 2.1 ev F. 3.2 ev G. Something else

Similar documents
Introduction to Electromagnetic Radiation and Radiative Transfer

Fluorescence Workshop UMN Physics June 8-10, 2006 Basic Spectroscopic Principles Joachim Mueller

Electromagnetic spectrum Electromagnetic radiation

Prof. Jeff Kenney Class 5 June 1, 2018

Particle nature of light & Quantization

Chapters 31 Atomic Physics

Quantum Theory of Light

Planck s Quantum Hypothesis Blackbody Radiation

1 The Cathode Rays experiment is associated. with: Millikan A B. Thomson. Townsend. Plank Compton

Chapter 4 Spectroscopy

Light & Atoms. Electromagnetic [EM] Waves. Light and several other forms of radiation are called electromagnetic waves or electromagnetic radiation.

Student Exploration: Bohr Model of Hydrogen

Light and Matter: Reading Messages from the Cosmos Pearson Education, Inc.

Review: Properties of a wave

Physics 107: Ideas of Modern Physics

Chapters 28 and 29: Quantum Physics and Atoms Questions & Problems

LECTURE 23 SPECTROSCOPY AND ATOMIC MODELS. Instructor: Kazumi Tolich

Department of Natural Sciences Clayton State University. Physics 3650 Quiz 1

Shell Atomic Model and Energy Levels

Classical and Planck picture. Planck s constant. Question. Quantum explanation for the Wein Effect.

Chapter 2 Problem Solutions

Light. October 14, ) Exam Review 2) Introduction 3) Light Waves 4) Atoms 5) Light Sources

Wave - Particle Duality of Light

Chapter 27. Quantum Physics

hf = E 1 - E 2 hc = E 1 - E 2 λ FXA 2008 Candidates should be able to : EMISSION LINE SPECTRA

From Last Time Pearson Education, Inc.

Chapter 28: Quantum Physics. Don t Copy This. Quantum Physics 3/16/13

PHYS 3313 Section 001 Lecture #7

Lecture Outline: Spectroscopy (Ch. 4)

Earlier we learned that hot, opaque objects produce continuous spectra of radiation of different wavelengths.

CHAPTER 27 Quantum Physics

10/27/2017 [pgs ]

Skoog Chapter 6 Introduction to Spectrometric Methods

Physics 102: Lecture 26. X-rays. Make sure your grade book entries are correct. Physics 102: Lecture 26, Slide 1

Properties of Electromagnetic Radiation Chapter 5. What is light? What is a wave? Radiation carries information

Rb, which had been compressed to a density of 1013

Chapter 4. Spectroscopy. Dr. Tariq Al-Abdullah

Atoms and Spectroscopy

Chapter 7. The Quantum Mechanical Model of the Atom

SPECTROSCOPY PRELAB. 2) Name the 3 types of spectra and, in 1 sentence each, describe them.

Lecture 15 Notes: 07 / 26. The photoelectric effect and the particle nature of light

Stellar Astrophysics: The Interaction of Light and Matter

II Light.

Carbon Dating The decay of radioactive nuclei can be used to measure the age of artifacts, fossils, and rocks. The half-life of C 14 is 5730 years.

HOMEWORK - Chapter 4 Spectroscopy

BCIT Fall Chem Exam #1

LASER. Challenging MCQ questions by The Physics Cafe. Compiled and selected by The Physics Cafe

Physics 102: Lecture 23

Chapter 38. Photons Light Waves Behaving as Particles

Chapter 27 Early Quantum Theory and Models of the Atom Discovery and Properties of the electron

Explain how Planck resolved the ultraviolet catastrophe in blackbody radiation. Calculate energy of quanta using Planck s equation.

The greenhouse effect

Light III The Atom & Spectra. February 12, 2012

Chapter 31 Atomic Physics

Wave properties of light

SECTION A Quantum Physics and Atom Models

Level 3 Physics: Atoms The Photoelectric Effect - Answers

From Last Time. Electron diffraction. Making a particle out of waves. Planetary model of atom. Using quantum mechanics ev 1/ 2 nm E kinetic

FXA UNIT G485 Module X-Rays. Candidates should be able to : I = I 0 e -μx

THE ELECTROMAGNETIC SPECTRUM. (We will go into more detail later but we need to establish some basic understanding here)

Particles and Waves Particles Waves

The Structure of the Atom

Wavelength of 1 ev electron

EMISSION AND ABSORPTION SPECTRUM

Spectroscopy. Hot self-luminous objects light the Sun or a light bulb emit a continuous spectrum of wavelengths.

Chapter 3. Electromagnetic Theory, Photons. and Light. Lecture 7

RED. BLUE Light. Light-Matter

PHYS General Physics II Lab The Balmer Series for Hydrogen Source. c = speed of light = 3 x 10 8 m/s

Physics 126 Practice Exam #4 Professor Siegel

Physics 102: Lecture 26. X-rays. Make sure your grade book entries are correct. Physics 102: Lecture 26, Slide 1

Chapters 28 and 29: Quantum Physics and Atoms Solutions

Quick Review. 1. Kinetic Molecular Theory. 2. Average kinetic energy and average velocity. 3. Graham s Law of Effusion. 4. Real Gas Behavior.

Physics 3204 UNIT 3 Test Matter Energy Interface

Quantum Mechanics (made fun and easy)

Class 21. Early Quantum Mechanics and the Wave Nature of Matter. Physics 106. Winter Press CTRL-L to view as a slide show. Class 21.

Chapter 28 Assignment Solutions

Chapter 27 Lecture Notes

Frequency: the number of complete waves that pass a point in a given time. It has the symbol f. 1) SI Units: Hertz (Hz) Wavelength: The length from

Semiconductor Physics and Devices

Models of the Atom. Spencer Clelland & Katelyn Mason

CHEM6416 Theory of Molecular Spectroscopy 2013Jan Spectroscopy frequency dependence of the interaction of light with matter

Review: Light and Spectra. Absorption and Emission Lines

English CPH E-Book Theory of CPH Section 2 Experimental Foundation of CPH Theory Hossein Javadi

Physics 6C. Photons. Prepared by Vince Zaccone For Campus Learning Assistance Services at UCSB

MIDTERM 3 REVIEW SESSION. Dr. Flera Rizatdinova

Physics 6C. The Photoelectric Effect. Prepared by Vince Zaccone For Campus Learning Assistance Services at UCSB

Unit 3. Chapter 4 Electrons in the Atom. Niels Bohr s Model. Recall the Evolution of the Atom. Bohr s planetary model

Lecture 5: the Hydrogen Atom

Preview. Atomic Physics Section 1. Section 1 Quantization of Energy. Section 2 Models of the Atom. Section 3 Quantum Mechanics

Chapter 30 Quantum Physics 30.1 Blackbody Radiation and Planck s Hypothesis of Quantum Energy 30.2 Photons and the Photoelectric Effect 30.

The Photoelectric Effect


LASER. Light Amplification by Stimulated Emission of Radiation

Chapter 37 Early Quantum Theory and Models of the Atom. Copyright 2009 Pearson Education, Inc.

THE NATURE OF THE ATOM. alpha particle source

The wavefunction ψ for an electron confined to move within a box of linear size L = m, is a standing wave as shown.

ATM S 111: Global Warming Solar Radiation. Jennifer Fletcher Day 2: June

LIGHT. Question. Until very recently, the study of ALL astronomical objects, outside of the Solar System, has been with telescopes observing light.

State the main interaction when an alpha particle is scattered by a gold nucleus

Particle Nature of Matter. Chapter 4

Transcription:

A molecule has the energy levels shown in the diagram at the right. We begin with a large number of these molecules in their ground states. We want to raise a lot of these molecules to the state labeled E 2 by shining light on it. What energy photon should we use? A. 0.7 ev B. 1.1 ev C. 1.4 ev D. 1.8 ev E. 2.1 ev F. 3.2 ev G. Something else 15

What is the wavelength of the light? E = hf f λ = c hc = 1234 ev-nm c = 3 10 8 m/s 16

A molecule has the energy levels shown in the diagram at the right. We have a large number of these molecules in the state E 2. The state decays by emitting photons. What might we expect about the wavelength of the emitted photons? A. They will be the same as the wavelength of the photons that were used to pump the molecules up to state E 2. B. Some might be the same wavelength, but some might be shorter. C. Some might be the same wavelength, but some might be longer. D. You only expect to see shorter wavelengths. E. You only expect to see longer wavelengths. F. You will see longer, shorter, and the same wavelengths. 17

A molecule has the energy levels shown in the diagram at the right. We have a large number of these molecules in the state E 2. The state decays by emitting photons. What energy photons might we expect to see? A. 0.7 ev B. 1.1 ev C. 1.4 ev D. 1.8 ev E. 2.1 ev F. 3.2 ev 1. B D F 2. B D 3. C 4. C E 5. A C E 6. Some other set 18

In the transitions you found in the last slide, which energy corresponds to the longest wavelength? (and what is it) A. 0.7 ev B. 1.4 ev C. 2.1 ev E = hf f λ = c hc = 1234 ev-nm c = 3 10 8 m/s 19

The jellyfish Aequorea Victoria creates a protein (GFP) that, when illuminated with blue light (λ = 395 nm) emits green light (λ = 508 nm). One way this conversion of frequencies could work is the following: A. The blue light is less energetic than the green light. The blue photon scatters off a protein and extracts energy from it, coming out green. B. The blue light is more energetic than the green light. The blue photon is absorbed by the protein, which then goes into a highly excited state. It decays back to the ground state in two stages, going through an intermediate excited state and emitting two photons of smaller energy, one of which is green. C. The protein acts as a prism, changing the wavelength of the blue light as it moves through the protein, stretching it into green light. D. The energy is not the relevant quantity. The blue light has a higher frequency than the green light. The blue light sets some of the electrons in the protein oscillating at a high frequency. The lower frequency is excited in conjunction with it in the way that a crystal goblet, rung by a pure tone, vibrates with other associated tones. 20 E. None of the above.

When high energy electrons are incident on a tungsten target, a broad spectrum of x-rays are given off. Most of the x-ray photons are spread over a range of energies, but there are a large number of x-rays with a specific energy -about 60 kev. This sharp x-ray line arises because: A. An electron bounces off a tungsten atom and since accelerating a charge leads to radiation, it gives off an x-ray when it does so. B. An electron excites a tungsten atom into a particular excited state and it gives off a particular x-ray when it returns to its original state. C. An electron slows via many collisions with electrons in many tungsten atoms. The combined effect of these collisions leads to the sharp x-ray line. D. An electron is absorbed by a nucleus of tungsten and converted into energy. E. None of the above. 21

Observations of an interstellar gas give an absorption spectrum, part of which is shown in the upper part of the figure. The gas is cold, such that when not excited, all electrons are in the ground state. Astronomers suspect the gas to be helium, but aren't sure. When they excite a sample of helium in the laboratory, they observe an emission spectrum, shown in the lower part of the figure below. Max says "line B cannot come from the same gas, or we would see it in the absorption spectrum. It must be from some other gas." Werner says, "I think that the same substance is responsible for all 5 lines. Who do you agree with? A. Max B. Werner C. Both D. Neither 22