AST 102 chapter 5. Radiation and Spectra. Radiation and Spectra. Radiation and Spectra. What is light? What is radiation?

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1 5 Radiation and Spectra 1 Radiation and Spectra What is light? According to Webster: a.something that makes vision possible b.the sensation aroused by stimulation of the visual receptors c.electromagnetic radiation of any wavelength that travels in a vacuum with a speed of about 186,281 miles (300,000 kilometers) per second; specifically: such radiation that is visible to the human eye 2 2 Radiation and Spectra What is radiation? According to Webster: a : the action or process of radiating b : the process of emitting energy c : the combined processes of emission, transmission, and absorption of radiant energy 3 3 1

2 Colors of Light Spectrum White light is made up of all the colors of the rainbow 4 Please read.. 5 Energy travels in waves Two types of waves Physical: travel through a medium A wave is an example of a physical wave Another example is : sound waves No swish as the Enterprise passes: vacuum Physical waves travel at different speeds 6 2

3 Energy travels in waves Two types of waves Electromagnetic: no medium required Radio Light All travel at same speed: speed of light 186,000 miles per second 7 Light waves are not all the same Differing colors Why? Answer: wavelength Wavelength (meters) Frequency (cycles per second or hertz) 8 Frequency: Number of wave crests that pass a given point per second Period: Time between passage of successive crests Relationship: Period = 1 / Frequency 9 3

4 Wavelength: Distance between successive crests Velocity: Speed at which crests move Relationship: Velocity = Wavelength / Period 10 Wavelength and Frequency What is GHz? wavelength frequency = speed of light = constant 11 Propagation of light Inverse-square law Light intensity will decrease by the square of the change in distance Double the distance, four times fainter Triple the distance, nine times fainter Ten times the distance, 100 times fainter 12 4

5 The Inverse-Square Law for Light The intensity of a 120W light bulb observed from a distance 2 meters away is 2.4 W/m 2. What would be the intensity if this distance was doubled? Solution If we move twice as far away, then the answer will change according to the inverse square of the distance, so the new intensity will be (1/2) 2 = 1/4 of the original intensity, or 0.6 W/m 2. Check Your Learning How many times brighter or fainter would a star appear if it were moved to: a. twice its present distance? (1/2) 2 = 1/4 b. ten times its present distance? (1/10) 2 = 1/100 c. half its present distance? 2 2 = 4 13 Propagation of light Inverse-square law For instance, the star Alpha Centauri emits as much light as our Sun, but is 270,000 times farther away. Therefore, it appears 73 billion times fainter. 14 Visible spectrum: small region! 15 5

6 Visible spectrum Covers all forms of electromagnetic radiation Types of electromagnetic radiation Gamma ray: shortest wavelength= high freq Radio waves: longest wavelength= low freq 17 Stars generate light and other forms of radiation by processes at the atomic level by the way atoms move and interact. 18 6

7 Universe must be studied at all wavelengths to get a complete picture Fig 5.7 shows the x-ray sky Red: glow from a hot local bubble of gas all around us Blue, yellow: more distant sources of X-rays, such as remnants of other exploded stars or the active center of our Galaxy 19 Table 5.1 (p. 156). Types of Electromagnetic Radiation 20 Problem: how can we study many wavelengths (x-rays, gamma rays, infrared) when they are absorbed by Earth's atmosphere? Only from orbit Hubble Space Telescope (mostly visual) Compton Gamma Ray Observatory Chandra X-Ray Observatory Spitzer Space Telescope (infrared) 21 7

8 5.3 Spectroscopy in Astronomy Optical properties of light Refraction Reflection Dispersion Spectroscopy in Astronomy Optical properties of light Dispersion Different wavelengths of light are refracted by different amounts The Rainbow Spectroscopy in Astronomy Spectrometer Breaks light up into spectrum 24 8

9 5.3 Spectroscopy in Astronomy Three types of Spectra Continuous Spectroscopy in Astronomy Three types of Spectra Absorption Dark lines Created by cooler gas in front of hotter gas (in Sun's outer atmosphere) Each chemical element has a signature set of lines, allowing scientists to determine composition of Sun or stars Spectroscopy in Astronomy Three types of Spectra Emission - bright lines Created by heated gas Fig

10 5.4 Structure of the Atom Nucleus Proton (+) Neutron (0) Electron (-) Charge must be balanced Structure of the Atom Hydrogen: simplest One proton, one electron, zero neutrons Structure of the Atom Helium, etc: also have neutrons in nucleus Helium = 2 neutrons, 2 protons, 2 electrons 30 10

11 5.4 Structure of the Atom Type of element is defined by the number of protons For instance, any atom with 6 protons is called carbon Isotopes: same number of protons, different number of neutrons Three hydrogen isotopes: Formation of Spectral Lines Ordinarily, atoms are at lowest energy level: ground state. As an atom absorbs energy, higher energy state: excited state. Electrons move to different orbital levels around the nucleus. Almost instantly returns to ground state, but in process, it emits radiation (light) Formation of Spectral Lines Each atomic element has its own unique pattern of electrons orbits, and no two sets of orbits are exactly alike. Therefore, each element shows its own unique set of spectral lines

12 Doppler Effect 1842: Christian Doppler Energy released by objects in motion is shifted slightly according to that motion. Toward us: shorter wavelength, higher pitch Away from us: longer wavelength, lower pitch Think railroad whistle Spectra of stars will show that shift as well Doppler Effect In the laboratory 36 12

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