1 Chapter 5 Light and Matter: Reading Messages from the Cosmos
2 5.1 Light in Everyday Life Our goals for learning How do we experience light? How do light and matter interact?
3 How do we experience light? The warmth of sunlight tells us that light is a form of energy We can measure the flow of energy in light in units of watts: 1 watt = 1 joule/s
4 Colors of Light White light is made up of many different colors
5 How do light and matter interact? Emission Absorption Transmission Transparent objects transmit light Opaque objects block (absorb) light Reflection or Scattering
6 Reflection and Scattering Mirror reflects light in a particular direction Movie screen scatters light in all directions
7 Interactions of Light with Matter Interactions between light and matter determine the appearance of everything around us
8 What have we learned? How do we experience light? Light is a form of energy Light comes in many colors that combine to form white light. How does light interact with matter? Matter can emit light, absorb light, transmit light, and reflect (or scatter) light. Interactions between light and matter determine the appearance of everything we see.
9 5.2 Properties of Light Our goals for learning What is light? What is the electromagnetic spectrum?
10 What is light? Light can act either like a wave or like a particle Particles of light are called photons
11 Waves A wave is a pattern of motion that can carry energy without carrying matter along with it
12 Properties of Waves Wavelength is the distance between two wave peaks Frequency is the number of times per second that a wave vibrates up and down wave speed = wavelength x frequency
13 Light: Electromagnetic Waves A light wave is a vibration of electric and magnetic fields Light interacts with charged particles through these electric and magnetic fields
14 Wavelength and Frequency wavelength x frequency = speed of light = constant
15 Particles of Light Particles of light are called photons Each photon has a wavelength and a frequency The energy of a photon depends on its frequency
16 Wavelength, Frequency, and Energy λ x f = c λ = wavelength, f = frequency c = 3.00 x 10 8 m/s = speed of light E = h x f = photon energy h = x joule x s = photon energy
17 Special Topic: Polarized Sunglasses Polarization describes the direction in which a light wave is vibrating Reflection can change the polarization of light Polarized sunglasses block light that reflects off of horizontal surfaces
18 What is the electromagnetic spectrum?
19 The Electromagnetic Spectrum
20 What have we learned? What is light? Light can behave like either a wave or a particle A light wave is a vibration of electric and magnetic fields Light waves have a wavelength and a frequency Photons are particles of light. What is the electromagnetic spectrum? Human eyes cannot see most forms of light. The entire range of wavelengths of light is known as the electromagnetic spectrum.
21 5.3 Properties of Matter Our goals for learning What is the structure of matter? What are the phases of matter How is energy stored in atoms?
22 What is the structure of matter? Electron Cloud Atom Nucleus
23 Atomic Terminology Atomic Number = # of protons in nucleus Atomic Mass Number = # of protons + neutrons Molecules: consist of two or more atoms (H 2 O, CO 2 )
24 Atomic Terminology Isotope:same # of protons but different # of neutrons. ( 4 He, 3 He)
25 What are the phases of matter? Familiar phases: Solid (ice) Liquid (water) Gas (water vapor) Phases of same material behave differently because of differences in chemical bonds
26 Phases of Water
27 Phase Changes Ionization: Stripping of electrons, changing atoms into plasma Dissociation: Breaking of molecules into atoms Evaporation: Breaking of flexible chemical bonds, changing liquid into solid Melting: Breaking of rigid chemical bonds, changing solid into liquid
28 Phases and Pressure Phase of a substance depends on both temperature and pressure Often more than one phase is present
29 How is energy stored in atoms? Excited States Ground State Electrons in atoms are restricted to particular energy levels
30 Energy Level Transitions The only allowed changes in energy are those corresponding to a transition between energy levels Not Allowed Allowed
31 What have we learned? What is the structure of matter? Matter is made of atoms, which consist of a nucleus of protons and neutrons surrounded by a cloud of electrons What are the phases of matter? Adding heat to a substance changes its phase by breaking chemical bonds. As temperature rises, a substance transforms from a solid to a liquid to a gas, then the molecules can dissociate into atoms Stripping of electrons from atoms (ionization) turns the substance into a plasma
32 What have we learned? How is energy stored in atoms? The energies of electrons in atoms correspond to particular energy levels. Atoms gain and lose energy only in amount corresponding to particular changes in energy levels.
33 5.4 Learning from Light Our goals for learning What are the three basic types of spectra? How does light tell us what things are made of? How does light tell us the temperatures of planets and stars? How do we interpret an actual spectrum?
34 What are the three basic types of spectra? Continuous Spectrum Emission Line Spectrum Absorption Line Spectrum Spectra of astrophysical objects are usually combinations of these three basic types
36 Three Types of Spectra
37 Continuous Spectrum The spectrum of a common (incandescent) light bulb spans all visible wavelengths, without interruption
38 Emission Line Spectrum A thin or low-density cloud of gas emits light only at specific wavelengths that depend on its composition and temperature, producing a spectrum with bright emission lines
39 Absorption Line Spectrum A cloud of gas between us and a light bulb can absorb light of specific wavelengths, leaving dark absorption lines in the spectrum
40 How does light tell us what things are made of? Spectrum of the Sun
41 Chemical Fingerprints Each type of atom has a unique set of energy levels Energy levels of Hydrogen Each transition corresponds to a unique photon energy, frequency, and wavelength
42 Chemical Fingerprints Downward transitions produce a unique pattern of emission lines
44 Chemical Fingerprints Because those atoms can absorb photons with those same energies, upward transitions produce a pattern of absorption lines at the same wavelengths
47 Chemical Fingerprints Each type of atom has a unique spectral fingerprint
49 Chemical Fingerprints Observing the fingerprints in a spectrum tells us which kinds of atoms are present
50 Example: Solar Spectrum
51 Energy Levels of Molecules Molecules have additional energy levels because they can vibrate and rotate
52 Energy Levels of Molecules Spectrum of Molecular Hydrogen The large numbers of vibrational and rotational energy levels can make the spectra of molecules very complicated Many of these molecular transitions are in the infrared part of the spectrum
53 How does light tell us the temperatures of planets and stars?
54 Thermal Radiation Nearly all large or dense objects emit thermal radiation, including stars, planets, you An object s thermal radiation spectrum depends on only one property: its temperature
55 Properties of Thermal Radiation 1. Hotter objects emit more light at all frequencies per unit area. 2. Hotter objects emit photons with a higher average energy.
56 Wien s Law
57 How do we interpret an actual spectrum? By carefully studying the features in a spectrum, we can learn a great deal about the object that created it.
58 What is this object? Reflected Sunlight: Continuous spectrum of visible light is like the Sun s except that some of the blue light has been absorbed - object must look red
59 What is this object? Thermal Radiation: Infrared spectrum peaks at a wavelength corresponding to a temperature of 225 K
60 What is this object? Carbon Dioxide: Absorption lines are the fingerprint of CO 2 in the atmosphere
61 What is this object? Ultraviolet Emission Lines: Indicate a hot upper atmosphere
62 What is this object? Mars!
63 What have we learned? What are the three basic type of spectra? Continuous spectrum, emission line spectrum, absorption line spectrum How does light tell us what things are made of? Each atom has a unique fingerprint. We can determine which atoms something is made of by looking for their fingerprints in the spectrum.
64 What have we learned? How does light tell us the temperatures of planets and stars? Nearly all large or dense objects emit a continuous spectrum that depends on temperature. The spectrum of that thermal radiation tells us the object s temperature. How do we interpret an actual spectrum? By carefully studying the features in a spectrum, we can learn a great deal about the object that created it.
65 5.5 The Doppler Effect Our goals for learning How does light tell us the speed of a distant object? How does light tell us the rotation rate of an object?
66 How does light tell us the speed of a distant object? The Doppler Effect
67 The Doppler Effect
68 Explaining the Doppler Effect
69 Same for Light
70 Measuring the Shift Stationary Moving Away Away Faster Moving Toward Toward Faster We generally measure the Doppler Effect from shifts in the wavelengths of spectral lines
71 The amount of blue or red shift tells us an object s speed toward or away from us:
72 Doppler shift tells us ONLY about the part of an object s motion toward or away from us:
73 Measuring Redshift
74 Measuring Redshift
75 Measuring Velocity
76 Measuring Velocity
77 How does light tell us the rotation rate of an object? Different Doppler shifts from different sides of a rotating object spread out its spectral lines
78 Spectrum of a Rotating Object Spectral lines are wider when an object rotates faster
79 What have we learned? How does light tell us the speed of a distant object? The Doppler effect tells us how fast an object is moving toward or away from us. Blueshift:objects moving toward us Redshift: objects moving away from us How does light tell us the rotation rate of an object? The width of an object s spectral lines can tell us how fast it is rotating
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