Buy-back points tallied and added: 750 points bought-back. Last Withdrawal date: this friday, Oct 31st.
|
|
- Alicia Dennis
- 5 years ago
- Views:
Transcription
1 Announcements HW #3: Available online now. Due in 1 week, Nov 3rd, 11pm. Buy-back points tallied and added: 750 points bought-back. Last Withdrawal date: this friday, Oct 31st. Evening Observing: next four nights, 8:30 9:45pm. WEATHER PERMITTING.
2 Of Sunspots and the Earth Question #1 on Exam 2: many of your secondguessed yourselves. Sunspots are about the same size as earth, some smaller, some bigger. But, figure 6.2 says a sunspot could swallow several earths. The biggest could. Since this was confusing, if you changed your correct answer in the buy-back extra-credit, you got full points (+2).
3 The image at right shows a picture of the Sun. The dark spots located on this image are sunspots. How does the size of Earth compare (approximately) to the size of the sunspot that is identified on the image of the Sun? Sunspot A) Earth and the sunspot are about the same size. B) The sunspot is much larger than Earth. C) The sunspot is much smaller than Earth.
4 The image at right shows a picture of the Sun. The dark spots located on this image are sunspots. How does the size of Earth compare (approximately) to the size of the sunspot that is identified on the image of the Sun? Sunspot A) Earth and the sunspot are about the same size. B) The sunspot is much larger than Earth. C) The sunspot is much smaller than Earth.
5 Last Time Light: carrier of information from the universe. Visible light just a tiny portion of all the electromagnetic spectrum. Even radio is a form of light. Light has a wavelength and frequency. High frequency=high energy=show wavelength, and visa versa.
6 Last Time Matter, composed of atoms, identified by atomic number (number of protons). This sets their properties. Isotopes have same number of protons, but different number of neutrons (e.g. Carbon 13). Light and matter interact by emission/ absorption/reflection/transmission.
7 Last Time The Spectrum of a source describes its intensity at each wavelength of light. There is a special spectrum of perfectly black emission, called blackbody. Most objects, including stars, emit a spectrum close to blackbody radiation. Hotter blackbody = shorter wavelength of peak emission.
8 The filter experiment (take 2) A red object absorbs all but red light. A red filter transmits all but red light.
9 High energy, short wavelength, high frequency Electromagnetic Spectrum Visible light: red, orange, yellow, green, blue, indigo, violet (ROY G BIV) Invisible Light: Ultraviolet = bluer than blue Infrared = redder than red (heat!) Other wavelengths: Short: X-rays, gamma-rays Long: microwave, radio Low energy, long wavelength, low frequency
10 Spectroscopy Prism separates light into different colors Continuous spectrum contains all colors Example: blackbody spectrum
11 Spectroscopy Absorption Line spectrum Some colors are missing (discrete lines)
12 The Solar Spectrum
13 The Solar Spectrum H Mg Na
14 Spectroscopy Emission Line spectrum Only certain colors are present (discrete lines) Spectrum for each element unique (like fingerprints)
15 How it Works
16 Thought question Which letter(s) mark absorption lines? A B C D E
17 Thought question Which letter(s) mark absorption lines? A B C D E
18 Thought question Which letter(s) mark Emission lines? A B C D E
19 Thought question Which letter(s) mark Emission lines? A B C D E
20 Doppler Shift (again) Just like a train, the pitch (frequency) of light changes if the light source is moving. Moving away: redshifted. Moving towards: blueshifted.
21 The Doppler Effect ONLY tells us the about an objects motion towards or away from us
22 Thought Question: You measure a line of hydrogen at nm in the lab. The same line has a wavelength of 659 nm in a star. The star: a) is moving away from you b) is moving towards you c) is not moving at all
23 Thought Question: You measure a line of hydrogen at nm in the lab. The same line has a wavelength of 659 nm in a star. The star: a) is moving away from you b) is moving towards you c) is not moving at all
24 Model Atom Electrons orbit nucleus Number of electrons = number of protons Ionization = removing electrons Only certain orbits are allowed hydrogen helium
25 Atomic Energy Levels In order to move between orbits (levels), the electron need gain or lose a specific amount of energy, and only that amount. level 3 level 2 level 1 1 H not to scale 1 ev (electron Volt) = 1.6 x J
26 Atomic Absorption Atom absorbs photon energy electron jumps to higher energy orbit only certain discrete orbits are allowed Atom can absorb only discrete colors (energies)
27 Atomic Emission Electron jumps to a lower energy orbit Atom emits photon can emit only discrete colors same colors (wavelengths/ energies) as absorption
28 Chemical Fingerprints each element or molecule has: a unique set of energy levels, and so a unique emission/absorption line spectrum we can determine the composition of a gas by looking at its spectrum!
29 Spectrum Demo Get a grating. Hold it up and look through it at the lamps. Should see various Rainbows going off in several directions. Please return at the top of the table, at the end of class.
30 Sun
31 Sun Hydrogen Helium Carbon Nitrogen Oxygen Neon Sodium Magnesium Aluminum Silicon
32 What can we learn Light can tell us: the temperature of an object. It s chemical composition (what it s made of!). Velocity of motion....much more (from across the universe!).
33 Workbook Time Analyzing Spectra, Page 69.
34 Consider the two spectral curves for Star V and Star Y shown in the graph at right. What can you determine about the relative temperatures of the two stars? A) Star V is at the higher temperature. B) Star Y is at the higher temperature. C) Both stars are the same temperature. D) The relative temperatures of the stars cannot be determined
35 Consider the two spectral curves for Star V and Star Y shown in the graph at right. What can you determine about the relative temperatures of the two stars? A) Star V is at the higher temperature. B) Star Y is at the higher temperature. C) Both stars are the same temperature. D) The relative temperatures of the stars cannot be determined
36 Red Hydrogen Line
37 Yellow Sodium Lines
38 Telescopes Eyes on the Heavens
39 What good are telescopes? Like giant light buckets, they collect more light than our eyes can (larger collecting area). They can see more detail than our eyes can (better resolution). They can detect other forms of light, like x- rays, infrared, radio (better wavelength coverage).
40 Bigger is better! Collects more light
41 Bigger is better! Better angular resolution 0.15 m 0.50 m Ability to separate two nearby objects. 2.4 m 5.0 m
42 Basic Telescope Design Refracting: lenses Refracting Telescope Yerkes 1-m refractor
43 Basic Telescope Design Reflecting: mirrors Reflecting Telescope Gemini 8 meter
44 Tom Jarrett
45 Mauna Kea, HI
46 Twin 10-m Keck Telescopes
47 Using telecopes Astronomers almost never look through a telescope with their eyes. Instead instruments are used which are more sensitive, can see other wavelengths of light, and can record their data directly are used.
48 Radio Telescopes
49 Why do we put telescopes in space? We can over come problems with the Earth s atmosphere
50 1.) Light Pollution
51 1.) Light Pollution Bright Sky Dark Sky
52 2) Atmospheric Turbulence Atmospheric turbulence causes twinkling which blurs the image Limits the angular resolution of all big telescopes to about 0.5 arcseconds
53 2) Atmospheric Turbulence Image 1: From sea level (3 arcseconds) Image 2: From a mountain (0.5 arcseconds) Image 3: Hubble Space Telescope (0.1 arcseconds)
54 3) Atmospheric Absorption Most radiation is absorbed by the atmosphere (which is a good thing!)
55
56 Technology & Astronomy Adaptive optics: A fast computer figures how the atmosphere is distorting the light and moves a deformable mirror to compensate.
57 Technology & Astronomy Interferometry: allows individual telescopes to work together to achieve the angular resolution of a larger telescope.
58 Very Large Array (New Mexico)
59 Reminders Hand in Gratings before you go! HW #3 due in 1 week. Observing this week. Check website for weather updates. Read Chapter 10 for next time!
Lecture Fall, 2005 Astronomy 110 1
Lecture 13+14 Fall, 2005 Astronomy 110 1 Important Concepts for Understanding Spectra Electromagnetic Spectrum Continuous Spectrum Absorption Spectrum Emission Spectrum Emission line Wavelength, Frequency
More informationChapter 5 Light: The Cosmic Messenger. Copyright 2012 Pearson Education, Inc.
Chapter 5 Light: The Cosmic Messenger 5.1 Basic Properties of Light and Matter Our goals for learning: What is light? What is matter? How do light and matter interact? What is light? Light is an electromagnetic
More information9/19/ Basic Properties of Light and Matter. Chapter 5: Light: The Cosmic Messenger. What is light? Lecture Outline
Lecture Outline 5.1 Basic Properties of Light and Matter Chapter 5: Light: The Cosmic Messenger Our goals for learning: What is light? What is matter? How do light and matter interact? What is light? Light
More informationTelescopes have Three Powers
Telescopes have Three Powers 1. Light Gathering Power: The ability to collect light 2. Resolving Power: The ability to see fine details 3. Magnifying Power: The ability to make objects look bigger Pizzas!!!
More informationNext Homework Due Oct. 9. Coming up: The Sun (Chapter 10)
Today Summary of Chapter 3: Light All of Chapter 4: Spectra & Atoms Optional: Ast. Toolbox 4-2 Optional: Stephan-Boltzmann Law Next Homework Due Oct. 9 Coming up: The Sun (Chapter 10) Resolving Power:
More informationChapter 6 Telescopes: Portals of Discovery. Agenda. How does your eye form an image? Refraction. Example: Refraction at Sunset
Chapter 6 Telescopes: Portals of Discovery Agenda Announce: Read S2 for Thursday Ch. 6 Telescopes 6.1 Eyes and Cameras: Everyday Light Sensors How does your eye form an image? Our goals for learning How
More informationChapter 6 Telescopes: Portals of Discovery
Chapter 6 Telescopes: Portals of Discovery 6.1 Eyes and Cameras: Everyday Light Sensors Our goals for learning: How does your eye form an image? How do we record images? How does your eye form an image?
More informationNext Homework Due March 6. Coming up: The Sun (Chapter 10)
Today Summary of Chapter 3: Light All of Chapter 4: Spectra & Atoms Optional: Ast. Toolbox 4-2 Optional: Stephan-Boltzmann Law Next Homework Due March 6 Coming up: The Sun (Chapter 10) Extra Credit Astro-talks:
More informationPHYS 160 Astronomy Test #2 Fall 2017 Version A
PHYS 160 Astronomy Test #2 Fall 2017 Version A I. True/False (1 point each) Circle the T if the statement is true, or F if the statement is false on your answer sheet. 1. A blackbody emits all of its radiation
More information(in case you missed it yesterday ) Merger of Two Neutron Stars!
(in case you missed it yesterday ) Merger of Two Neutron Stars! https://cmns.umd.edu/news-events/features/3997 More on this later in the semester Lecture #14: Plan Light (cont d) Atomic physics Formation
More informationRefraction is the bending of light when it passes from one substance into another. Your eye uses refraction to focus light.
Telescopes Portals of Discovery Chapter 6 Lecture The Cosmic Perspective 6.1 Eyes and Cameras: Everyday Light Sensors How do eyes and cameras work? Seventh Edition Telescopes Portals of Discovery The Eye
More informationLight and Atoms. ASTR 1120 General Astronomy: Stars & Galaxies. ASTR 1120 General Astronomy: Stars & Galaxies !ATH REVIEW: #AST CLASS: "OMEWORK #1
ASTR 1120 General Astronomy: Stars & Galaxies!ATH REVIEW: Tonight, 5-6pm, in RAMY N1B23 "OMEWORK #1 -Due THU, Sept. 10, by 5pm, on Mastering Astronomy CLASS RECORDED STARTED - INFO WILL BE POSTED on CULEARN
More informationTelescopes: Portals of Discovery Pearson Education, Inc.
Telescopes: Portals of Discovery 6.1 Eyes and Cameras: Everyday Light Sensors Our goals for learning: How do eyes and cameras work? The Eye Refraction Incoming light ray Air Glass Refraction is the bending
More informationProperties of Thermal Radiation
Observing the Universe: Telescopes Astronomy 2020 Lecture 6 Prof. Tom Megeath Today s Lecture: 1. A little more on blackbodies 2. Light, vision, and basic optics 3. Telescopes Properties of Thermal Radiation
More informationSummary. Week 7: 10/5 & 10/ Learning from Light. What are the three basic types of spectra? Three Types of Spectra
Week 7: 10/5 & 10/7 Capturing that radiation Chapter 6 (Telescopes & Sensors) Optical to Radio Summary What are we sensing? Matter! Matter is made of atoms (nucleus w/ protons, neutrons & cloud of electrons
More information1. Using, scientists can use a few smaller telescopes to take images with the. 2. To double the resolving power of a telescope, you must.
Chapter 5 Telescopes Multiple Choice Questions 1. Using, scientists can use a few smaller telescopes to take images with the same resolution as a much larger telescope. A. Satellite telescopes B. Charge-coupled
More informationAssignments. For Mon. 1 st Midterm is Friday, Oct. 12. Read Ch. 6 Optionally do MT1-sample-problems
Assignments For Mon. Read Ch. 6 Optionally do MT1-sample-problems 1 st Midterm is Friday, Oct. 12 Chapter 5 Light: The Cosmic Messenger Thermal Radiation 1. Hotter objects emit photons with a higher average
More informationChapter 5: Light and Matter: Reading Messages from the Cosmos
Chapter 5 Lecture Chapter 5: Light and Matter: Reading Messages from the Cosmos Light and Matter: Reading Messages from the Cosmos 5.1 Light in Everyday Life Our goals for learning: How do we experience
More information7. Telescopes: Portals of Discovery Pearson Education Inc., publishing as Addison Wesley
7. Telescopes: Portals of Discovery Parts of the Human Eye pupil allows light to enter the eye lens focuses light to create an image retina detects the light and generates signals which are sent to the
More informationTopics for Today. Clicker Q: Radio Waves. Radios. Discussion of how do ROTATING STARS yield Doppler-broadened spectral emission lines
ASTR 1040 Accel Astro: Stars & Galaxies Topics for Today Basic principles of eyes, camera, telescopes Twinkle and absorption by our atmosphere What light gets through, what does not Next lecture: Telescopes
More informationChapter 5 Light and Matter: Reading Messages from the Cosmos. How do we experience light? Colors of Light. How do light and matter interact?
Chapter 5 Light and Matter: Reading Messages from the Cosmos How do we experience light? The warmth of sunlight tells us that light is a form of energy We can measure the amount of energy emitted by a
More informationAST 102 chapter 5. Radiation and Spectra. Radiation and Spectra. Radiation and Spectra. What is light? What is radiation?
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
More informationWhat are the most important properties of a telescope? Chapter 6 Telescopes: Portals of Discovery. What are the two basic designs of telescopes?
Chapter 6 Telescopes: Portals of Discovery What are the most important properties of a telescope? 1. Light-collecting area: Telescopes with a larger collecting area can gather a greater amount of light
More informationChapter 5 Light and Matter: Reading Messages from the Cosmos. 5.1 Light in Everyday Life. How do we experience light?
Chapter 5 Light and Matter: Reading Messages from the Cosmos 5.1 Light in Everyday Life Our goals for learning: How do we experience light? How do light and matter interact? How do we experience light?
More informationAST 101 Intro to Astronomy: Stars & Galaxies
AST 101 Intro to Astronomy: Stars & Galaxies Telescopes Mauna Kea Observatories, Big Island, HI Imaging with our Eyes pupil allows light to enter the eye lens focuses light to create an image retina detects
More informationWhat is LIGHT? Reading Question
Reading Question What is LIGHT? A. Light is a wave, like sound only much faster. B. Light is like little particles. Each one is a photon. C. Light is the absence of dark. D. A kind of energy we model with
More informationName: Partner(s): 1102 or 3311: Desk # Date: Spectroscopy Part I
Name: Partner(s): 1102 or 3311: Desk # Date: Spectroscopy Part I Purpose Investigate Kirchhoff s Laws for continuous, emission and absorption spectra Analyze the solar spectrum and identify unknown lines
More informationAstronomy 1 Fall 2016
Astronomy 1 Fall 2016 One person s perspective: Three great events stand at the threshold of the modern age and determine its character: 1) the discovery of America; 2) the Reformation; 3) the invention
More informationHow does your eye form an Refraction
Astronomical Instruments Eyes and Cameras: Everyday Light Sensors How does your eye form an image? How do we record images? How does your eye form an image? Refraction Refraction is the bending of light
More informationToday. Next time. Emission & Absorption lines measuring elemental abundances. Doppler Effect. Telescopes technology to measure with
Today Emission & Absorption lines measuring elemental abundances Doppler Effect measuring motion Telescopes technology to measure with Solar System Overview what s out there? Next time Homework 3 Due Chemical
More informationFinal Announcements. Lecture25 Telescopes. The Bending of Light. Parts of the Human Eye. Reading: Chapter 7. Turn in the homework#6 NOW.
Final Announcements Turn in the homework#6 NOW. Homework#5 and Quiz#6 will be returned today. Today is the last lecture. Lecture25 Telescopes Reading: Chapter 7 Final exam on Thursday Be sure to clear
More informationAST 105 Intro Astronomy The Solar System. MIDTERM II: Tuesday, April 5 [covering Lectures 10 through 16]
AST 105 Intro Astronomy The Solar System MIDTERM II: Tuesday, April 5 [covering Lectures 10 through 16] REVIEW Light as Information Bearer We can separate light into its different wavelengths (spectrum).
More informationSPECTROSCOPY PRELAB. 2) Name the 3 types of spectra and, in 1 sentence each, describe them.
NAME: SPECTROSCOPY PRELAB 1) What is a spectrum? 2) Name the 3 types of spectra and, in 1 sentence each, describe them. a. b. c. 3) Use Wien s law to calculate the surface temperature of the star Alnilam
More informationPrentice Hall EARTH SCIENCE
Prentice Hall EARTH SCIENCE Tarbuck Lutgens Chapter 24 Studying the Sun 24.1 The Study of Light Electromagnetic Radiation Electromagnetic radiation includes gamma rays, X-rays, ultraviolet light, visible
More informationReview: Properties of a wave
Radiation travels as waves. Waves carry information and energy. Review: Properties of a wave wavelength (λ) crest amplitude (A) trough velocity (v) λ is a distance, so its units are m, cm, or mm, etc.
More informationASTRONOMY. Chapter 5 RADIATION AND SPECTRA PowerPoint Image Slideshow
ASTRONOMY Chapter 5 RADIATION AND SPECTRA PowerPoint Image Slideshow FIGURE 5.1 Our Sun in Ultraviolet Light. This photograph of the Sun was taken at several different wavelengths of ultraviolet, which
More informationX Rays must be viewed from space used for detecting exotic objects such as neutron stars and black holes also observing the Sun.
6/25 How do we get information from the telescope? 1. Galileo drew pictures. 2. With the invention of photography, we began taking pictures of the view in the telescope. With telescopes that would rotate
More informationPhases of ma*er strongly depend on temperature
Phases of ma*er strongly depend on temperature Light and Atoms Remember that each electron is only allowed to have certain energies in an atom. Electrons can absorb light and gain energy or emit light
More informationWhat are the three basic types of spectra?
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
More informationFrom Last Time Pearson Education, Inc.
From Last Time Light: Absorption, Emission, Transmission, Reflection, and Scattering c=λ x f E=h x f Light (electromagnetic radiation) extends from gamma rays (high E, high f, small λ) to radio waves (small
More informationToday. Doppler Effect & Motion. Telescopes
Today Doppler Effect & Motion Telescopes The Doppler Effect Doppler ball 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley Doppler Effect for Light Motion away -> redshift Motion towards
More informationThe Basics of Light. Sunrise from the Space Shuttle, STS-47 mission. The Basics of Light
The Basics of Light The sun as it appears in X-ray light (left) and extreme ultraviolet light (right). Light as energy Light is remarkable. It is something we take for granted every day, but it's not something
More informationStars, Galaxies & the Universe (29:50) Professor C.C. Lang Exam #1 - Fall 2010 Wednesday, September 22 nd FORM B - SOLUTIONS
Stars, Galaxies & the Universe (29:50) Professor C.C. Lang Exam #1 - Fall 2010 Wednesday, September 22 nd FORM B - SOLUTIONS Questions 1-6 are True/False questions (worth 4 pts each): 1. The Sun is a Red
More informationChapter 6 Light and Telescopes
Chapter 6 Light and Telescopes Guidepost In the early chapters of this book, you looked at the sky the way ancient astronomers did, with the unaided eye. In chapter 4, you got a glimpse through Galileo
More informationLight and Matter: Reading Messages from the Cosmos. White light is made up of many different colors. Interactions of Light with Matter
Chapter 5 Lecture The Cosmic Perspective Light and Matter: Reading Messages from the Cosmos 5.1 Light in Everyday Life Our goals for learning: How do we experience light? How do light and matter interact?
More informationASTR 1120 General Astronomy: Stars & Galaxies
ASTR 1120 General Astronomy: Stars & Galaxies!AST CLASS Learning from light: temperature (from continuum spectrum) chemical composition (from spectral lines) velocity (from Doppler shift) "ODA# Detecting
More informationChapter 6 Lecture. The Cosmic Perspective Seventh Edition. Telescopes Portals of Discovery Pearson Education, Inc.
Chapter 6 Lecture The Cosmic Perspective Seventh Edition Telescopes Portals of Discovery Telescopes Portals of Discovery 6.1 Eyes and Cameras: Everyday Light Sensors Our goals for learning: How do eyes
More informationOn to Telescopes. Imaging with our Eyes. Telescopes and cameras work much like our eyes. ASTR 1120 General Astronomy: Stars & Galaxies !
ASTR 1120 General Astronomy: Stars & Galaxies On to Telescopes!AST CLASS Learning from light: temperature (from continuum spectrum) chemical composition (from spectral lines) velocity (from Doppler shift)
More informationThe Theory of Electromagnetism
Notes: Light The Theory of Electromagnetism James Clerk Maxwell (1831-1879) Scottish physicist. Found that electricity and magnetism were interrelated. Moving electric charges created magnetism, changing
More informationAtoms and Spectra October 8th, 2013
Atoms and Spectra October 8th, 2013 Announcements Second writing assignment due two weeks from today (again, on a news item of your choice). Be sure to make plans to visit one of the open observing nights
More information@astro_stephi. Telescopes. CAASTRO in the Classroom: National Science Week Stephanie Bernard, University of Melbourne
@astro_stephi Telescopes CAASTRO in the Classroom: National Science Week 2017 Stephanie Bernard, University of Melbourne About me NASA, ESA NASA, JPL The first telescopes Invented in 1600s in the Netherlands
More informationToday. Spectra. Thermal Radiation. Wien s Law. Stefan-Boltzmann Law. Kirchoff s Laws. Emission and Absorption. Spectra & Composition
Today Spectra Thermal Radiation Wien s Law Stefan-Boltzmann Law Kirchoff s Laws Emission and Absorption Spectra & Composition Spectrum Originally, the range of colors obtained by passing sunlight through
More informationChapter 6 Lecture. The Cosmic Perspective. Telescopes Portals of Discovery Pearson Education, Inc.
Chapter 6 Lecture The Cosmic Perspective Telescopes Portals of Discovery 2014 Pearson Education, Inc. Telescopes Portals of Discovery CofC Observatory 6.1 Eyes and Cameras: Everyday Light Sensors Our goals
More informationHow does your eye form an Refraction
Astronomical Instruments and : Everyday Light Sensors How does your eye form an image? How do we record images? How does your eye form an image? Refraction Refraction is the of light Eye uses refraction
More informationSusan Cartwright Our Evolving Universe 1
Atoms and Starlight Why do the stars shine? planets shine by reflected sunlight but what generates the Sun s light? What does starlight tell us about the stars? their temperature their chemical composition
More informationAssignments. For Wed. 1 st Midterm is Friday, Oct. 12. Do Online Exercise 08 ( Doppler shift tutorial)
Assignments For Wed. Do Online Exercise 08 ( Doppler shift tutorial) 1 st Midterm is Friday, Oct. 12 Chapter 5 Light: The Cosmic Messenger Which forms of light are lower in energy and frequency than the
More informationChapter 5 Light and Matter
Chapter 5 Light and Matter Stars and galaxies are too far for us to send a spacecraft or to visit (in our lifetimes). All we can receive from them is light But there is much we can learn (composition,
More informationToday. Kirchoff s Laws. Emission and Absorption. Stellar Spectra & Composition. Doppler Effect & Motion. Extrasolar Planets
Today Kirchoff s Laws Emission and Absorption Stellar Spectra & Composition Doppler Effect & Motion Extrasolar Planets Three basic types of spectra Continuous Spectrum Intensity Emission Line Spectrum
More informationDoppler Shifts. Doppler Shift Lecture-Tutorial: Pgs Temperature or Heat? What can we learn from light? Temp: Peak in Thermal Radiation
Doppler Shift Lecture-Tutorial: Pgs. 75-80 Work with a partner or two Read directions and answer all questions carefully. Take time to understand it now! Come to a consensus answer you all agree on before
More information= λ. Light: The Cosmic Messenger. Continuing Topics for Today 1/24/17. Your account on Mastering Astronomy. ASTR 1040 Stars & Galaxies
REMINDER Your account on Mastering Astronomy ASTR 1040 Stars & Galaxies SDO: Post-flare ejection from solar surface Prof. Juri Toomre TAs: Piyush Agrawal, Connor Bice Lecture 3 Tues 24 Jan 2017 zeus.colorado.edu/astr1040-toomre
More informationLecture Outline: Spectroscopy (Ch. 4)
Lecture Outline: Spectroscopy (Ch. 4) NOTE: These are just an outline of the lectures and a guide to the textbook. The material will be covered in more detail in class. We will cover nearly all of the
More informationAST 101 INTRODUCTION TO ASTRONOMY SPRING MIDTERM EXAM 1 TEST VERSION 1 ANSWERS NOTE: Question 20 Fixed
AST 101 INTRODUCTION TO ASTRONOMY SPRING 2008 - MIDTERM EXAM 1 TEST VERSION 1 ANSWERS NOTE: Question 20 Fixed Multiple Choice. In the blanks provided before each question write the letter for the phrase
More informationTelescopes. Telescopes Key Concepts. glass
Telescopes Telescopes Key Concepts 1) A refracting telescope uses a lens to gather light; a reflecting telescope uses a mirror. ) The main purposes of a telescope are to gather light and resolve fine detail.
More informationIntro to Galaxies Light and Atoms - I
Astrophysics Study of Light Study of Atoms Intro to Galaxies Light and Atoms - I 1 Atomic Physics elements: substances which cannot be broken down into simpler substances atom : smallest unit of an element
More informationLights. And God said, "Let there be light"; and there was light. And God saw that the light was good; (Bible: Genesis I)
Lights Astronomy is based on observing lights from celestial bodies. And God said, "Let there be light"; and there was light. And God saw that the light was good; (Bible: Genesis I) Cat's Eye planetary
More informationAgenda Announce: Visions of Science Visions of Science Winner
7. Telescopes: Portals of Discovery All of this has been discovered and observed these last days thanks to the telescope that I have [built], after having been enlightened by divine grace. Galileo Galilei
More informationCollecting Light. In a dark-adapted eye, the iris is fully open and the pupil has a diameter of about 7 mm. pupil
Telescopes Collecting Light The simplest means of observing the Universe is the eye. The human eye is sensitive to light with a wavelength of about 400 and 700 nanometers. In a dark-adapted eye, the iris
More informationChapter 5 Light and Matter: Reading Messages from the Cosmos
Chapter 5 Light and Matter: Reading Messages from the Cosmos 5.1 Light in Everyday Life Our goals for learning How do we experience light? How do light and matter interact? How do we experience light?
More information! Finish Ch. 4.! Start Chapter 10: The Sun.! Homework Due: Oct. 10
! Finish Ch. 4! Start Chapter 10: The Sun! Homework Due: Oct. 10 A Spectral Mystery Mystery: Why do so many stars have an absorption spectrum (with certain colors missing)? The atoms that make up these
More information9/16/08 Tuesday. Chapter 3. Properties of Light. Light the Astronomer s Tool. and sometimes it can be described as a particle!
9/16/08 Tuesday Announce: Observations? Milky Way Center movie Moon s Surface Gravity movie Questions on Gravity from Ch. 2 Ch. 3 Newton Movie Chapter 3 Light and Atoms Copyright (c) The McGraw-Hill Companies,
More informationAstronomy. Optics and Telescopes
Astronomy A. Dayle Hancock adhancock@wm.edu Small 239 Office hours: MTWR 10-11am Optics and Telescopes - Refraction, lenses and refracting telescopes - Mirrors and reflecting telescopes - Diffraction limit,
More informationLIGHT. Question. Until very recently, the study of ALL astronomical objects, outside of the Solar System, has been with telescopes observing light.
LIGHT Question Until very recently, the study of ALL astronomical objects, outside of the Solar System, has been with telescopes observing light. What kind of information can we get from light? 1 Light
More informationASTR-1010: Astronomy I Course Notes Section IV
ASTR-1010: Astronomy I Course Notes Section IV Dr. Donald G. Luttermoser Department of Physics and Astronomy East Tennessee State University Edition 2.0 Abstract These class notes are designed for use
More informationChapter 5 Light and Matter: Reading Messages from the Cosmos. What is light? Properties of Waves. Waves. The Electromagnetic Spectrum
Chapter 5 Light and Matter: Reading Messages from the Cosmos What is light? Light is a form of radiant energy Light can act either like a wave or like a particle (photon) Spectrum of the Sun 1 2 Waves
More informationNext quiz: Monday, October 24 Chp. 6 (nothing on telescopes) Chp. 7 a few problems from previous material cough, cough, gravity, cough, cough...
Next quiz: Monday, October 24 Chp. 6 (nothing on telescopes) Chp. 7 a few problems from previous material cough, cough, gravity, cough, cough... 1 Chapter 7 Atoms and Starlight Kirchhoff s Laws of Radiation
More informationThe Nature of Light. We have a dual model
Light and Atoms Properties of Light We can come to understand the composition of distant bodies by analyzing the light they emit This analysis can tell us about the composition as well as the temperature
More informationAnswer Key for Exam C
Answer Key for Exam C 1 point each Choose the answer that best completes the question. Read each problem carefully and read through all the answers. Take your time. If a question is unclear, ask for clarification
More informationAnswer Key for Exam B
Answer Key for Exam B 1 point each Choose the answer that best completes the question. Read each problem carefully and read through all the answers. Take your time. If a question is unclear, ask for clarification
More informationTypes of Spectra. How do spectrum lines form? 3/30/09. Electron cloud. Atom. Nucleus
The electron should be thought of as a distribution or cloud of probability around the nucleus that on average behave like a point particle on a fixed circular path Types of Spectra How do spectrum lines
More informationPhys 100 Astronomy (Dr. Ilias Fernini) Review Questions for Chapter 5
Phys 100 Astronomy (Dr. Ilias Fernini) Review Questions for Chapter 5 MULTIPLE CHOICE 1. What is the wavelength of the longest wavelength light visible to the human eye? a. 400 nm b. 4000 nm c. 7000 nm
More informationLight Pollution. Atmospheric Seeing. Seeing Through the Atmosphere. Atmospheric Absorption of Light
Lec 8: 2 FEB 2012 ASTR 130 - Introductory Astronomy II (Chapter 6) LAST TIME - Optics and Telescopes Basic Functions of a Telescope Reflecting v. Refracting Affects of the Atmosphere TODAY Modern Astronomical
More informationMidterm Exam. IT Posting scores Finding out about missed questions Reminder about dropping lowest of 3
Midterm Exam #&%?@)#$! IT Posting scores Finding out about missed questions Reminder about dropping lowest of 3 Nature of Light 10/3 Apparent versus Actual Brightness 10/6 Electromagnetic Spectrum of Light
More informationAtoms and Spectroscopy
Atoms and Spectroscopy Lecture 3 1 ONE SMALL STEP FOR MAN ONE GIANT LEAP FOR MANKIND 2 FROM ATOMS TO STARS AND GALAXIES HOW DO WE KNOW? Observations The Scientific Method Hypothesis Verifications LAW 3
More informationTelescopes and the Atmosphere
Telescopes and the Atmosphere Our goals for learning How does Earth s atmosphere affect ground-based observations? Why do we put telescopes into space? How does Earth s atmosphere affect ground-based observations?
More informationChapter 4 Spectroscopy
Chapter 4 Spectroscopy The beautiful visible spectrum of the star Procyon is shown here from red to blue, interrupted by hundreds of dark lines caused by the absorption of light in the hot star s cooler
More informationProf. Jeff Kenney Class 5 June 1, 2018
www.astro.yale.edu/astro120 Prof. Jeff Kenney Class 5 June 1, 2018 to understand how we know stuff about the universe we need to understand: 1. the spectral analysis of light 2. how light interacts with
More informationFoundations of Astronomy 13e Seeds. Chapter 6. Light and Telescopes
Foundations of Astronomy 13e Seeds Chapter 6 Light and Telescopes Guidepost In this chapter, you will consider the techniques astronomers use to study the Universe What is light? How do telescopes work?
More informationLight and Matter(LC)
Light and Matter(LC) Every astronomy book that I ve seen has at least one chapter dedicated to the physics of light. Why are astronomers so interested in light? Everything* that we know about Astronomical
More informationAstronomy 1504/15014 Section 20
1 point each Astronomy 1504/15014 Section 20 Midterm 1 (Practice Exam) September 21, 2015 Exam Version A Choose the answer that best completes the question. Read each problem carefully and read through
More informationc = l Light: The Cosmic Messenger 1/23/18
Reading for today s and Thur class: ASTR 1040 Stars & Galaxies SDO: Post-flare ejection from solar surface Prof. Juri Toomre TAs: Peri Johnson, Ryan Horton Lecture 3 Tues 23 Jan 2018 zeus.colorado.edu/astr1040-toomre
More informationChapter 23. Light, Astronomical Observations, and the Sun
Chapter 23 Light, Astronomical Observations, and the Sun The study of light Electromagnetic radiation Visible light is only one small part of an array of energy Electromagnetic radiation includes Gamma
More informationAstronomy 101 Test 1 Review FOUNDATIONS
Astronomy 101 Test 1 Review FOUNDATIONS Scientists use the metric system to measure things. It is based on powers ten, and is thus more logical than our everyday Imperial system. The kilogram (or gram),
More informationReading for Meaning and the Electromagnetic Spectrum!
Earth Science Zimmerman Name: Period: Reading for Meaning and the Electromagnetic Spectrum! HOOK: An astronomer discovers a new galaxy. How can the Doppler Effect be applied to determine if that galaxy
More information= λ. Topics for Today. Clicker Q: Radio Waves. Radios. Light Pollution. Problems in Looking Through Our Atmosphere
ASTR 1040 Accel Astro: Stars & Galaxies Prof. Juri Toomre TA: Nick Featherstone Lecture 5 Tues 30 Jan 07 zeus.colorado.edu/astr1040-toomre toomre Topics for Today Twinkle and absorption by our atmosphere
More informationEx: N has 5 valence electrons, so it s Lewis structure would look like: N
Chemistry Ms. Ye Review: Bohr Model of the Atom Name Date Block Electrons are shown in concentric shells or energy levels around the nucleus o The first shell can hold up to o The second shell can hold
More informationThe Electromagnetic Spectrum
The Electromagnetic Spectrum Learning Objectives! What is Electromagnetic Radiation?! What are spectra? How could we measure a spectrum?! How do wavelengths correspond to colors for optical light? Does
More informationASTRO Fall 2012 LAB #7: The Electromagnetic Spectrum
ASTRO 1050 - Fall 2012 LAB #7: The Electromagnetic Spectrum ABSTRACT Astronomers rely on light to convey almost all of the information we have on distant astronomical objects. In addition to measuring
More informationDiscussion Review Test #2. Units 12-19: (1) (2) (3) (4) (5) (6)
Discussion Review Test #2 Units 12-19: (1) (2) (3) (4) (5) (6) (7) (8) (9) Galileo used his observations of the changing phases of Venus to demonstrate that a. the sun moves around the Earth b. the universe
More informationLecture #8. Light-matter interaction. Kirchoff s laws
1 Lecture #8 Light-matter interaction Kirchoff s laws 2 Line emission/absorption Atoms: release and absorb photons with a predefined set of energies (discrete). The number of protons determine the chemical
More informationLecture #15: Plan. Telescopes (cont d) Effects of Earth s Atmosphere Extrasolar planets = Exoplanets
Lecture #15: Plan Telescopes (cont d) Effects of Earth s Atmosphere Extrasolar planets = Exoplanets Collecting Area Light bucket : the bigger the area of the telescope s mirror or lens, the more photons
More information