7. What is chromatic aberration in a telescope? (b) The light of different colors comes to a focus at different points inside the telescope.
|
|
- Bertina Martin
- 7 years ago
- Views:
Transcription
1 ASTR 1020 Stellar and Galactic Astronomy Professor Caillault Fall 2009 Semester Exam 2 Multiple Choice Answers (Each multiple choice question is worth 1.5 points) 1. Light enters the smooth, flat surface of a glass from the vacuum of space (e.g., a spacecraft window). What is the speed of light inside the glass compared to that in a vacuum? (b) Since the glass is denser than the vacuum, it is slower. 2. What is the refraction of light? (d) The change in direction of a light ray as it crosses from a less dense, transparent material to a more dense one 3. A typical refracting telescope is made up of (a) a long-focal-length lens at the front and a short-focal-length lens at the rear (next to your eye as you look through the telescope). 4. When light from the concave primary mirror of a telescope is reflected by a small secondary mirror through a hole in the primary, it is called a (c) Cassegrain focus telescope. 5. A refracting telescope has an objective lens of focal length 80 cm, a diameter of 10 cm, and an eyepiece of focal length 5 cm and diameter 1 cm. What is the magnifying power of this telescope? (c) For many years, the Palomar telescope (5 m diameter) in California was the largest fully steerable telescope in the world; in the 1990 s that honor fell to the first of the two Keck telescopes (each of diameter 10 m) in Hawaii. How many times larger is the lightgathering power of a Keck telescope than the Palomar telescope? (c) 4 times larger 7. What is chromatic aberration in a telescope? (b) The light of different colors comes to a focus at different points inside the telescope. 8. The largest refracting telescope in the world is the 102-cm (40 in.) diameter telescope at Yerkes Observatory, built in Refracting telescopes with larger diameter have never been built because they would (a) sag too much under their own weight. 9. A reflecting telescope in which light is reflected by one curved mirror and a second plane mirror at 45 to the original beam, to reach a focus at the side of the telescope, is being used at its (a) Newtonian focus.
2 10. A spherical mirror suffers from spherical aberration because (c) different parts of the mirror focus the light at different distances from the mirror. 11. In telescopes, the angular resolution is worse for (d) smaller diameter lenses or mirrors and longer wavelength electromagnetic radiation. 12. What does the word seeing mean to an astronomer using a telescope? (a) The twinkling and blurring of the image due to air currents in Earth's atmosphere. 13. During the past few decades a number of techniques have been developed to enhance the performance of optical and radio telescopes. These include all of the following except one. Which one is the exception? (b) building refracting telescopes comparable in size to the largest reflecting telescopes 14. What is the main reason for combining many radio telescopes together into an interferometer with large distances between telescopes? (a) to obtain much sharper images of sources 15. When four protons collide to form helium, what fraction of the original mass of the protons is converted to energy? (b) 0.7% 16. How much longer can the Sun continue to generate energy by nuclear reactions in its core? (c) about 5 billion years 17. What happens to the positrons produced by the nuclear reactions in the core of the Sun? (a) They are annihilated upon interacting with electrons, producing energy. 18. What happens to the neutrinos produced by the nuclear reactions in the core of the Sun? (d) They escape from the Sun into space. 19. Hydrogen burning by fusion reactions occurs only in the deep interior of the Sun (and other stars), because this is the only place in the Sun where (d) the requisite conditions of high temperature and high density occur. 20. The phrase hydrostatic equilibrium in the Sun refers to (d) the balance of gravity inward and gas pressure outward. 21. The solution to the solar neutrino problem is thought to be that (b) neutrinos oscillate and change their nature en route from the Sun to the Earth. 22. When we look at the Sun, what do we see? (c) Its photosphere.
3 23. The granulation pattern seen on the surface of the Sun results from (d) convection of gas in the region under the photosphere. 24. The center of the disk of the visible Sun appears brighter than its edges because (b) we see into deeper and hotter layers at the center of the solar disk. 25. The extremely high gas temperatures in the solar corona mean that this region is best observed at wavelengths of (d) X-rays. 26. What causes sunspots? (d) Magnetic fields inhibit gas motion in regions of the convective zone where the field is strong, lowering the amount of heat transferred to the surface. 27. What is the average length of time from one maximum in the number of sunspots on the Sun to the next maximum? (d) 11 years 28. The Zeeman effect refers to (d) the splitting of spectral lines when magnetic fields are applied to atoms. 29. The Babcock magnetic-dynamo model, which explains many of the features of the solar cycle, makes use of which two basic properties of the Sun s photosphere? (d) convection and differential rotation 30. The spectrum of an ordinary main sequence star is a (a) continuum of colors crossed by dark absorption lines, caused by absorption of cooler atoms and molecules at the surface. 31. Stellar parallax is the (d) apparent shift in the position of a nearby star because of Earth's motion. 32. The spectral class of the Sun is G2 and the star Enif is K2. From this information, we know that Enif is (c) cooler than the Sun. 33. What does apparent magnitude tell us about a star? (c) the brightness of a star as it appears in our sky 34. Star A has a luminosity L A = 100 L o and it is 1000 pc away. Star B has the same luminosity as the Sun, L A = 1 L o, and it is 100 pc away. What can you say about the brightnesses of these two stars? (d) Star A and Star B have the same brightness.
4 35. The Hertzsprung-Russell diagram is a plot of (d) luminosity vs. temperature. 36. What is the physical reason that astronomers can find the luminosity class (I, II, III, IV, or V) of a star using the star's spectrum? (b) The absorption lines in the spectrum are affected by the density and pressure of the star's atmosphere. 37. Spectroscopic parallax is the (d) distance to a star measured using the spectral-luminosity class of the star and the inverse square law. 38. The star Elnath is classified as B7 III, and the star Al Na'ir is classified as B7 IV. This tells us that compared to Al Na'ir, Elnath is (d) about the same temperature, but intrinsically much brighter. 39. Which important stellar parameter can be determined only by the study of binary stars? (b) mass 40. Which of the following pairs of stars is an example of stars for which the massluminosity relation applies? (a) G2 V and M1 V. 41. A radial-velocity curve is a plot of (a) radial-velocity vs. time for a spectroscopic binary. 42. What physical parameter of a star is usually determined indirectly, but with an eclipsing binary can be measured directly? (b) radius 43. What is the predominant atomic or molecular mechanism that produces the light we see from emission nebulae? (d) UV light from hot stars ionizes atoms, and the subsequent recombination of electrons with these ions produces spectral lines. 44. The distinct blue color of the nebulosity around stars in young clusters, such as the Pleiades, is caused by (b) preferential scattering of blue starlight by small dust grains in the interstellar material. 45. Suppose the light leaving a star has equal intensities in the blue and the red. The starlight passes through a dust cloud on its journey to Earth. When you observe the light reaching Earth you will find (b) the red part of the spectrum will be more intense than the blue.
5 46. The source of a protostar's heat is (a) gravitational energy, released as the protostar contracts. 47. At what point in its evolution will a protostar stop shrinking and stabilize into a star? (a) when nuclear processes generate enough energy and internal pressure to resist gravitational contraction. 48. A star's evolutionary track is (a) its movement when plotted on a HR diagram, as it evolves in luminosity and temperature. 49. What is the relationship between the mass of a protostar and the time needed for it to reach the main sequence, after it forms inside an interstellar cloud? (a) More massive protostars reach the main sequence in a shorter time than less massive protostars. 50. If we plot the stars in a 10 million year old star cluster on a Hertzsprung-Russell diagram, we would expect to see (d) the more massive stars on the main sequence and the less massive stars above the main sequence.
6 ASTR 1020 Stellar and Galactic Astronomy Professor Caillault Fall 2009 Semester Exam 2 Problems Solutions (Each problem is worth 5 points; show all of your work!) 1. If all effects caused by Earth's atmospheric variations (i.e., seeing) could be removed from the visible image of a star obtained with one of the 10-m diameter Keck telescopes on Hawaii, what would be the angular resolution achievable by this telescope for light of wavelength 500 nm? (Give your answer in arcseconds.) θ = ( )λ/d = ( )( m)/(10 m) = arcseconds = The mass of a hydrogen nucleus = kg. The mass of a helium nucleus = kg. How much energy is released by the formation of a single helium nucleus in the proton-proton chain? The proton-proton chain results in 4 H He + E, so E = (m 4H m He )c 2 = (( kg) kg)( m/s) 2 = J Consider a star with an apparent magnitude of and a parallax angle of arcseconds. 3. What is the distance to this star? d = 1/p = 1/ (0.010) = 100 pc 4. What is the absolute magnitude of this star? Is this star intrinsically brighter or fainter than the Sun (the Sun s absolute magnitude = +4.8)? m M = 5 log d 5, so rewrite to solve for absolute magnitude M: M = m 5 log d + 5 = log (100) + 5 = 12.1 (5 2) + 5 = 7.1 The star is intrinsically fainter than the Sun since its absolute magnitude is larger.
7 5. At one stage during its pre-main sequence phase, the protosun had a luminosity equal to 100 L o and a surface temperature of about 2900 K (= ½ T o ). At that time what was the protosun s radius (in terms of the Sun s present-day radius, R o )? Since L = 4πR 2 σ T 4, we know that L protosun = 4π(R protosun ) 2 σ(t protosun ) 4 and L o = 4πR o2 σt o4. Take the ratio: L protosun /L o = [4π(R protosun ) 2 σ(t protosun ) 4 ]/[4πR o 2 σt o 4 ] = [(R protosun ) 2 /R o2 ] [(T protosun ) 4 /T o4 ] Solve for R protosun /R o : R protosun /R o = [T o2 / (T protosun ) 2 ] (L protosun /L o ) = [T o2 /(½ T o ) 2 ] (100 L o /L o ) = 4 10 = 40
7. In which part of the electromagnetic spectrum are molecules most easily detected? A. visible light B. radio waves C. X rays D.
1. Most interstellar matter is too cold to be observed optically. Its radiation can be detected in which part of the electromagnetic spectrum? A. gamma ray B. ultraviolet C. infrared D. X ray 2. The space
More informationLecture 14. Introduction to the Sun
Lecture 14 Introduction to the Sun ALMA discovers planets forming in a protoplanetary disc. Open Q: what physics do we learn about the Sun? 1. Energy - nuclear energy - magnetic energy 2. Radiation - continuum
More informationClass 2 Solar System Characteristics Formation Exosolar Planets
Class 1 Introduction, Background History of Modern Astronomy The Night Sky, Eclipses and the Seasons Kepler's Laws Newtonian Gravity General Relativity Matter and Light Telescopes Class 2 Solar System
More informationOrigins of the Cosmos Summer 2016. Pre-course assessment
Origins of the Cosmos Summer 2016 Pre-course assessment In order to grant two graduate credits for the workshop, we do require you to spend some hours before arriving at Penn State. We encourage all of
More informationScience Standard 4 Earth in Space Grade Level Expectations
Science Standard 4 Earth in Space Grade Level Expectations Science Standard 4 Earth in Space Our Solar System is a collection of gravitationally interacting bodies that include Earth and the Moon. Universal
More informationUsing Photometric Data to Derive an HR Diagram for a Star Cluster
Using Photometric Data to Derive an HR Diagram for a Star Cluster In In this Activity, we will investigate: 1. How to use photometric data for an open cluster to derive an H-R Diagram for the stars and
More informationSolar Ast ro p h y s ics
Peter V. Foukal Solar Ast ro p h y s ics Second, Revised Edition WI LEY- VCH WILEY-VCH Verlag Co. KCaA Contents Preface 1 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 2 2.1 2.1.1 2.1.2 2.2 2.2.1 2.2.2 2.2.3 2.3
More information8.1 Radio Emission from Solar System objects
8.1 Radio Emission from Solar System objects 8.1.1 Moon and Terrestrial planets At visible wavelengths all the emission seen from these objects is due to light reflected from the sun. However at radio
More informationTHE HR DIAGRAM THE MOST FAMOUS DIAGRAM in ASTRONOMY Mike Luciuk
THE HR DIAGRAM THE MOST FAMOUS DIAGRAM in ASTRONOMY Mike Luciuk 1.INTRODUCTION Late in the nineteenth century, astronomers had tools that revealed a great deal about stars. By that time, advances in telescope
More informationSTAAR Science Tutorial 30 TEK 8.8C: Electromagnetic Waves
Name: Teacher: Pd. Date: STAAR Science Tutorial 30 TEK 8.8C: Electromagnetic Waves TEK 8.8C: Explore how different wavelengths of the electromagnetic spectrum such as light and radio waves are used to
More informationCosmic Journey: Teacher Packet
Cosmic Journey: Teacher Packet Compiled by: Morehead State University Star Theatre with help from Bethany DeMoss Table of Contents Table of Contents 1 Corresponding Standards 2 Vocabulary 4 Sizing up the
More informationBe Stars. By Carla Morton
Be Stars By Carla Morton Index 1. Stars 2. Spectral types 3. B Stars 4. Be stars 5. Bibliography How stars are formed Stars are composed of gas Hydrogen is the main component of stars. Stars are formed
More informationFrom lowest energy to highest energy, which of the following correctly orders the different categories of electromagnetic radiation?
From lowest energy to highest energy, which of the following correctly orders the different categories of electromagnetic radiation? From lowest energy to highest energy, which of the following correctly
More informationTest 2 --- Natural Sciences 102, Professors Rieke --- VERSION B March 3, 2010
Enter your answers on the form provided. Be sure to write your name and student ID number on the first blank at the bottom of the form. Please mark the version (B) in the Key ID space at the top of the
More informationThis paper is also taken for the relevant Examination for the Associateship. For Second Year Physics Students Wednesday, 4th June 2008: 14:00 to 16:00
Imperial College London BSc/MSci EXAMINATION June 2008 This paper is also taken for the relevant Examination for the Associateship SUN, STARS, PLANETS For Second Year Physics Students Wednesday, 4th June
More informationMain sequence stars. Haris Ðapo. Antalya Lecture 3. 1 Akdeniz University, Antalya
Main sequence stars Haris Ðapo 1 Akdeniz University, Antalya Antalya Lecture 3. Haris Ðapo (Akdeniz University) Main sequence stars Main sequence stars 1 / 22 Outline 1 Introduction 2 Hydrogen burning
More informationHomework #4 Solutions ASTR100: Introduction to Astronomy Fall 2009: Dr. Stacy McGaugh
Homework #4 Solutions ASTR100: Introduction to Astronomy Fall 2009: Dr. Stacy McGaugh Chapter 5: #50 Hotter Sun: Suppose the surface temperature of the Sun were about 12,000K, rather than 6000K. a. How
More information165 points. Name Date Period. Column B a. Cepheid variables b. luminosity c. RR Lyrae variables d. Sagittarius e. variable stars
Name Date Period 30 GALAXIES AND THE UNIVERSE SECTION 30.1 The Milky Way Galaxy In your textbook, read about discovering the Milky Way. (20 points) For each item in Column A, write the letter of the matching
More informationUNIT V. Earth and Space. Earth and the Solar System
UNIT V Earth and Space Chapter 9 Earth and the Solar System EARTH AND OTHER PLANETS A solar system contains planets, moons, and other objects that orbit around a star or the star system. The solar system
More informationThe Sun and Solar Energy
I The Sun and Solar Energy One of the most important forces behind global change on Earth is over 90 million miles distant from the planet. The Sun is the ultimate, original source of the energy that drives
More informationStellar Evolution: a Journey through the H-R Diagram
Stellar Evolution: a Journey through the H-R Diagram Mike Montgomery 21 Apr, 2001 0-0 The Herztsprung-Russell Diagram (HRD) was independently invented by Herztsprung (1911) and Russell (1913) They plotted
More informationIn studying the Milky Way, we have a classic problem of not being able to see the forest for the trees.
In studying the Milky Way, we have a classic problem of not being able to see the forest for the trees. A panoramic painting of the Milky Way as seen from Earth, done by Knut Lundmark in the 1940 s. The
More informationChapter 17: Light and Image Formation
Chapter 17: Light and Image Formation 1. When light enters a medium with a higher index of refraction it is A. absorbed. B. bent away from the normal. C. bent towards from the normal. D. continues in the
More informationNuclear fusion in stars. Collapse of primordial density fluctuations into galaxies and stars, nucleosynthesis in stars
Nuclear fusion in stars Collapse of primordial density fluctuations into galaxies and stars, nucleosynthesis in stars The origin of structure in the Universe Until the time of formation of protogalaxies,
More informationIntroduction to Astronomy. Lecture 4: Our star, the Sun
Introduction to Astronomy Lecture 4: Our star, the Sun 1 Sun Facts Age = 4.6 x 10 9 years Mean Radius = 7.0x10 5 km = 1.1x10 2 R = 1R Volume = 1.4x10 18 km 3 = 1.3x10 6 R = 1V Mass = 2x10 30 kg = 3.3x10
More informationLight Telescopes. Grade Level: 5. 2-3 class periods (more if in-depth research occurs)
Light Telescopes Grade Level: 5 Time Required: Suggested TEKS: Science - 5.4 Suggested SCANS Information. Acquires and evaluates information. National Science and Math Standards Science as Inquiry, Earth
More informationObserving the Universe
Observing the Universe Stars & Galaxies Telescopes Any questions for next Monday? Light Doppler effect Doppler shift Doppler shift Spectra Doppler effect Spectra Stars Star and planet formation Sun Low-mass
More information1 Introduction. Name: 1.1 Spectral Classification of Stars. PHYS-1050 Hertzsprung-Russell Diagram Solutions Spring 2013
Name: 1 Introduction Read through this information before proceeding on with the lab. 1.1 Spectral Classification of Stars 1.1.1 Types of Spectra Astronomers are very interested in spectra graphs of intensity
More informationStellar Evolution. The Basic Scheme
Stellar Evolution The Basic Scheme Stars live for a very long time compared to human lifetimes. Even though stellar life-spans are enormous, we know how stars are born, live, and die. All stars follow
More informationThe Birth of the Universe Newcomer Academy High School Visualization One
The Birth of the Universe Newcomer Academy High School Visualization One Chapter Topic Key Points of Discussion Notes & Vocabulary 1 Birth of The Big Bang Theory Activity 4A the How and when did the universe
More information5. The Nature of Light. Does Light Travel Infinitely Fast? EMR Travels At Finite Speed. EMR: Electric & Magnetic Waves
5. The Nature of Light Light travels in vacuum at 3.0. 10 8 m/s Light is one form of electromagnetic radiation Continuous radiation: Based on temperature Wien s Law & the Stefan-Boltzmann Law Light has
More informationCalifornia Standards Grades 9 12 Boardworks 2009 Science Contents Standards Mapping
California Standards Grades 912 Boardworks 2009 Science Contents Standards Mapping Earth Sciences Earth s Place in the Universe 1. Astronomy and planetary exploration reveal the solar system s structure,
More informationChapter 6 Telescopes: Portals of Discovery. How does your eye form an image? Refraction. Example: Refraction at Sunset.
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 informationScience Focus 9 Space Exploration Topic Test
SPACE EXPLORATION UNIT TEST ASSESSMENT Student Name Class 1. The axis for the frame of reference to identify locations on the earth are A. Equinox and Solstice B. Ecuador and Madagascar C. Equator and
More informationMultiple Choice Identify the choice that best completes the statement or answers the question.
Test 2 f14 Multiple Choice Identify the choice that best completes the statement or answers the question. 1. Carbon cycles through the Earth system. During photosynthesis, carbon is a. released from wood
More informationAstro 102 Test 5 Review Spring 2016. See Old Test 4 #16-23, Test 5 #1-3, Old Final #1-14
Astro 102 Test 5 Review Spring 2016 See Old Test 4 #16-23, Test 5 #1-3, Old Final #1-14 Sec 14.5 Expanding Universe Know: Doppler shift, redshift, Hubble s Law, cosmic distance ladder, standard candles,
More informationLight. What is light?
Light What is light? 1. How does light behave? 2. What produces light? 3. What type of light is emitted? 4. What information do you get from that light? Methods in Astronomy Photometry Measure total amount
More informationData Provided: A formula sheet and table of physical constants is attached to this paper. DARK MATTER AND THE UNIVERSE
Data Provided: A formula sheet and table of physical constants is attached to this paper. DEPARTMENT OF PHYSICS AND ASTRONOMY Autumn Semester (2014-2015) DARK MATTER AND THE UNIVERSE 2 HOURS Answer question
More informationWHERE DID ALL THE ELEMENTS COME FROM??
WHERE DID ALL THE ELEMENTS COME FROM?? In the very beginning, both space and time were created in the Big Bang. It happened 13.7 billion years ago. Afterwards, the universe was a very hot, expanding soup
More informationClassroom Exercise ASTR 390 Selected Topics in Astronomy: Astrobiology A Hertzsprung-Russell Potpourri
Classroom Exercise ASTR 390 Selected Topics in Astronomy: Astrobiology A Hertzsprung-Russell Potpourri Purpose: 1) To understand the H-R Diagram; 2) To understand how the H-R Diagram can be used to follow
More informationLight as a Wave. The Nature of Light. EM Radiation Spectrum. EM Radiation Spectrum. Electromagnetic Radiation
The Nature of Light Light and other forms of radiation carry information to us from distance astronomical objects Visible light is a subset of a huge spectrum of electromagnetic radiation Maxwell pioneered
More informationSolar Nebula Theory. Basic properties of the Solar System that need to be explained:
Solar Nebula Theory Basic properties of the Solar System that need to be explained: 1. All planets orbit the Sun in the same direction as the Sun s rotation 2. All planetary orbits are confined to the
More informationStudy Guide for Exam on Light
Name: Class: Date: Study Guide for Exam on Light Multiple Choice Identify the choice that best completes the statement or answers the question. 1. Which portion of the electromagnetic spectrum is used
More informationWELCOME to Aurorae In the Solar System. J.E. Klemaszewski
WELCOME to Aurorae In the Solar System Aurorae in the Solar System Sponsoring Projects Galileo Europa Mission Jupiter System Data Analysis Program ACRIMSAT Supporting Projects Ulysses Project Outer Planets
More informationa) species of plants that require a relatively cool, moist environment tend to grow on poleward-facing slopes.
J.D. McAlpine ATMS 611 HMWK #8 a) species of plants that require a relatively cool, moist environment tend to grow on poleward-facing slopes. These sides of the slopes will tend to have less average solar
More informationPractice final for Basic Physics spring 2005 answers on the last page Name: Date:
Practice final for Basic Physics spring 2005 answers on the last page Name: Date: 1. A 12 ohm resistor and a 24 ohm resistor are connected in series in a circuit with a 6.0 volt battery. Assuming negligible
More informationUnit 8 Lesson 2 Gravity and the Solar System
Unit 8 Lesson 2 Gravity and the Solar System Gravity What is gravity? Gravity is a force of attraction between objects that is due to their masses and the distances between them. Every object in the universe
More informationFXA 2008. UNIT G485 Module 5 5.5.1 Structure of the Universe. Δλ = v λ c CONTENTS OF THE UNIVERSE. Candidates should be able to :
1 Candidates should be able to : CONTENTS OF THE UNIVERSE Describe the principal contents of the universe, including stars, galaxies and radiation. Describe the solar system in terms of the Sun, planets,
More informationUNIVERSITY OF SASKATCHEWAN Department of Physics and Engineering Physics
UNIVERSITY OF SASKATCHEWAN Department of Physics and Engineering Physics Physics 111.6 MIDTERM TEST #4 March 15, 2007 Time: 90 minutes NAME: (Last) Please Print (Given) STUDENT NO.: LECTURE SECTION (please
More informationSKINAKAS OBSERVATORY. Astronomy Projects for University Students PROJECT THE HERTZSPRUNG RUSSELL DIAGRAM
PROJECT 4 THE HERTZSPRUNG RUSSELL DIGRM Objective: The aim is to measure accurately the B and V magnitudes of several stars in the cluster, and plot them on a Colour Magnitude Diagram. The students will
More informationSolar Energy Production
Solar Energy Production We re now ready to address the very important question: What makes the Sun shine? Why is this such an important topic in astronomy? As humans, we see in the visible part of the
More informationLecture 10 Formation of the Solar System January 6c, 2014
1 Lecture 10 Formation of the Solar System January 6c, 2014 2 Orbits of the Planets 3 Clues for the Formation of the SS All planets orbit in roughly the same plane about the Sun. All planets orbit in the
More informationHoward Eskildsen often uploads some of his wonderful and exquisite solar
Solar Images Taken with Calcium K-Line Filters Howard L. Cohen January 2014 (Rev. March 2015) Howard Eskildsen s beautiful images of the Sun uploaded to the AAC website may appear strange and unfamiliar
More informationA Universe of Galaxies
A Universe of Galaxies Today s Lecture: Other Galaxies (Chapter 16, pages 366-397) Types of Galaxies Habitats of Galaxies Dark Matter Other Galaxies Originally called spiral nebulae because of their shape.
More informationAy 122 - Fall 2004. The Sun. And The Birth of Neutrino Astronomy. This printout: Many pictures missing, in order to keep the file size reasonable
Ay 122 - Fall 2004 The Sun And The Birth of Neutrino Astronomy This printout: Many pictures missing, in order to keep the file size reasonable Why Study the Sun? The nearest star - can study it in a greater
More informationThe Expanding Universe
Stars, Galaxies, Guided Reading and Study This section explains how astronomers think the universe and the solar system formed. Use Target Reading Skills As you read about the evidence that supports the
More informationastronomy 2008 1. A planet was viewed from Earth for several hours. The diagrams below represent the appearance of the planet at four different times.
1. A planet was viewed from Earth for several hours. The diagrams below represent the appearance of the planet at four different times. 5. If the distance between the Earth and the Sun were increased,
More informationMaking a reflector telescope
Making a reflector telescope telescope built by Sir Isaac Newton Replica of the first reflector Nowadays, professional astronomers use another type of telescope that is different to the first telescope
More informationName Class Date. true
Exercises 131 The Falling Apple (page 233) 1 Describe the legend of Newton s discovery that gravity extends throughout the universe According to legend, Newton saw an apple fall from a tree and realized
More informationModeling Galaxy Formation
Galaxy Evolution is the study of how galaxies form and how they change over time. As was the case with we can not observe an individual galaxy evolve but we can observe different galaxies at various stages
More informationLight and its effects
Light and its effects Light and the speed of light Shadows Shadow films Pinhole camera (1) Pinhole camera (2) Reflection of light Image in a plane mirror An image in a plane mirror is: (i) the same size
More informationThe Earth s Atmosphere
THE SUN-EARTH SYSTEM III The Earth s Atmosphere Composition and Distribution of the Atmosphere The composition of the atmosphere and the way its gases interact with electromagnetic radiation determine
More informationSTUDY GUIDE: Earth Sun Moon
The Universe is thought to consist of trillions of galaxies. Our galaxy, the Milky Way, has billions of stars. One of those stars is our Sun. Our solar system consists of the Sun at the center, and all
More informationOverview. What is EMR? Electromagnetic Radiation (EMR) LA502 Special Studies Remote Sensing
LA502 Special Studies Remote Sensing Electromagnetic Radiation (EMR) Dr. Ragab Khalil Department of Landscape Architecture Faculty of Environmental Design King AbdulAziz University Room 103 Overview What
More informationPhysical Science Study Guide Unit 7 Wave properties and behaviors, electromagnetic spectrum, Doppler Effect
Objectives: PS-7.1 Physical Science Study Guide Unit 7 Wave properties and behaviors, electromagnetic spectrum, Doppler Effect Illustrate ways that the energy of waves is transferred by interaction with
More informationExplain the Big Bang Theory and give two pieces of evidence which support it.
Name: Key OBJECTIVES Correctly define: asteroid, celestial object, comet, constellation, Doppler effect, eccentricity, eclipse, ellipse, focus, Foucault Pendulum, galaxy, geocentric model, heliocentric
More informationAstronomy 110 Homework #04 Assigned: 02/06/2007 Due: 02/13/2007. Name:
Astronomy 110 Homework #04 Assigned: 02/06/2007 Due: 02/13/2007 Name: Directions: Listed below are twenty (20) multiple-choice questions based on the material covered by the lectures this past week. Choose
More information1051-232 Imaging Systems Laboratory II. Laboratory 4: Basic Lens Design in OSLO April 2 & 4, 2002
05-232 Imaging Systems Laboratory II Laboratory 4: Basic Lens Design in OSLO April 2 & 4, 2002 Abstract: For designing the optics of an imaging system, one of the main types of tools used today is optical
More informationSYLLABUS FORM WESTCHESTER COMMUNITY COLLEGE Valhalla, NY l0595. l. Course #:PHYSC 151 2. NAME OF ORIGINATOR /REVISOR: PAUL ROBINSON
SYLLABUS FORM WESTCHESTER COMMUNITY COLLEGE Valhalla, NY l0595 l. Course #:PHYSC 151 2. NAME OF ORIGINATOR /REVISOR: PAUL ROBINSON NAME OF COURSE: ASTRONOMY 3. CURRENT DATE: OCTOBER 26, 2011. Please indicate
More informationLenses and Telescopes
A. Using single lenses to form images Lenses and Telescopes The simplest variety of telescope uses a single lens. The image is formed at the focus of the telescope, which is simply the focal plane of the
More informationChapter 6 Formation of Planetary Systems Our Solar System and Beyond
Chapter 6 Formation of Planetary Systems Our Solar System and Beyond The solar system exhibits clear patterns of composition and motion. Sun Over 99.9% of solar system s mass Made mostly of H/He gas (plasma)
More informationIV. Molecular Clouds. 1. Molecular Cloud Spectra
IV. Molecular Clouds Dark structures in the ISM emit molecular lines. Dense gas cools, Metals combine to form molecules, Molecular clouds form. 1. Molecular Cloud Spectra 1 Molecular Lines emerge in absorption:
More informationPTYS/ASTR 206 Section 2 Spring 2007 Homework #2 (Page 1/5) NAME: KEY
PTYS/ASTR 206 Section 2 Spring 2007 Homework #2 (Page 1/5) NAME: KEY Due Date: start of class 2/6/2007 5 pts extra credit if turned in before 9:00AM (early!) (To get the extra credit, the assignment must
More informationElectromagnetic Radiation (EMR) and Remote Sensing
Electromagnetic Radiation (EMR) and Remote Sensing 1 Atmosphere Anything missing in between? Electromagnetic Radiation (EMR) is radiated by atomic particles at the source (the Sun), propagates through
More informationDemonstration of Data Analysis using the Gnumeric Spreadsheet Solver to Estimate the Period for Solar Rotation
Demonstration of Data Analysis using the Gnumeric Spreadsheet Solver to Estimate the Period for Solar Rotation Ron Larham Hart Plain Institute for Studies Introduction This paper serves two purposes, the
More informationL3: The formation of the Solar System
credit: NASA L3: The formation of the Solar System UCL Certificate of astronomy Dr. Ingo Waldmann A stable home The presence of life forms elsewhere in the Universe requires a stable environment where
More informationBlackbody radiation. Main Laws. Brightness temperature. 1. Concepts of a blackbody and thermodynamical equilibrium.
Lecture 4 lackbody radiation. Main Laws. rightness temperature. Objectives: 1. Concepts of a blackbody, thermodynamical equilibrium, and local thermodynamical equilibrium.. Main laws: lackbody emission:
More informationFirst let us consider microscopes. Human eyes are sensitive to radiation having wavelengths between
Optical Differences Between Telescopes and Microscopes Robert R. Pavlis, Girard, Kansas USA icroscopes and telescopes are optical instruments that are designed to permit observation of objects and details
More informationSolar Energy. Outline. Solar radiation. What is light?-- Electromagnetic Radiation. Light - Electromagnetic wave spectrum. Electromagnetic Radiation
Outline MAE 493R/593V- Renewable Energy Devices Solar Energy Electromagnetic wave Solar spectrum Solar global radiation Solar thermal energy Solar thermal collectors Solar thermal power plants Photovoltaics
More informationThe Sun: Our nearest star
The Sun: Our nearest star Property Surface T Central T Luminosity Mass Lifetime (ms) Value 5500K 15x10 6 K 2 x 10 33 ergs 4 x 10 33 grams 10 billion years Solar Structure Build a model and find the central
More information1. You stand two feet away from a plane mirror. How far is it from you to your image? a. 2.0 ft c. 4.0 ft b. 3.0 ft d. 5.0 ft
Lenses and Mirrors 1. You stand two feet away from a plane mirror. How far is it from you to your image? a. 2.0 ft c. 4.0 ft b. 3.0 ft d. 5.0 ft 2. Which of the following best describes the image from
More informationHow To Understand Light And Color
PRACTICE EXAM IV P202 SPRING 2004 1. In two separate double slit experiments, an interference pattern is observed on a screen. In the first experiment, violet light (λ = 754 nm) is used and a second-order
More informationStudy Guide due Friday, 1/29
NAME: Astronomy Study Guide asteroid chromosphere comet corona ellipse Galilean moons VOCABULARY WORDS TO KNOW geocentric system meteor gravity meteorite greenhouse effect meteoroid heliocentric system
More informationModeling the Expanding Universe
H9 Modeling the Expanding Universe Activity H9 Grade Level: 8 12 Source: This activity is produced by the Universe Forum at NASA s Office of Space Science, along with their Structure and Evolution of the
More information2 Absorbing Solar Energy
2 Absorbing Solar Energy 2.1 Air Mass and the Solar Spectrum Now that we have introduced the solar cell, it is time to introduce the source of the energy the sun. The sun has many properties that could
More informationLecture 7 Formation of the Solar System. Nebular Theory. Origin of the Solar System. Origin of the Solar System. The Solar Nebula
Origin of the Solar System Lecture 7 Formation of the Solar System Reading: Chapter 9 Quiz#2 Today: Lecture 60 minutes, then quiz 20 minutes. Homework#1 will be returned on Thursday. Our theory must explain
More informationBeginning of the Universe Classwork 6 th Grade PSI Science
Beginning of the Universe Classwork Name: 6 th Grade PSI Science 1 4 2 5 6 3 7 Down: 1. Edwin discovered that galaxies are spreading apart. 2. This theory explains how the Universe was flattened. 3. All
More informationSummary: Four Major Features of our Solar System
Summary: Four Major Features of our Solar System How did the solar system form? According to the nebular theory, our solar system formed from the gravitational collapse of a giant cloud of interstellar
More informationIndiana's Academic Standards 2010 ICP Indiana's Academic Standards 2016 ICP. map) that describe the relationship acceleration, velocity and distance.
.1.1 Measure the motion of objects to understand.1.1 Develop graphical, the relationships among distance, velocity and mathematical, and pictorial acceleration. Develop deeper understanding through representations
More informationDIRECT ORBITAL DYNAMICS: USING INDEPENDENT ORBITAL TERMS TO TREAT BODIES AS ORBITING EACH OTHER DIRECTLY WHILE IN MOTION
1 DIRECT ORBITAL DYNAMICS: USING INDEPENDENT ORBITAL TERMS TO TREAT BODIES AS ORBITING EACH OTHER DIRECTLY WHILE IN MOTION Daniel S. Orton email: dsorton1@gmail.com Abstract: There are many longstanding
More information- the. or may. scales on. Butterfly wing. magnified about 75 times.
Lecture Notes (Applications of Diffraction) Intro: - the iridescent colors seen in many beetles is due to diffraction of light rays hitting the small groovess of its exoskeleton - these ridges are only
More informationAppropriate space vocabulary for Primary School
Appropriate space vocabulary for Primary School Stuff Looks like Gas Dust Rock Liquid Fatter (moon) Thinner (moon) Faster Slower Hot Cold Material Shape Straight at (an object) Direct (light) Indirect
More informationYour years of toil Said Ryle to Hoyle Are wasted years, believe me. The Steady State Is out of date Unless my eyes deceive me.
Your years of toil Said Ryle to Hoyle Are wasted years, believe me. The Steady State Is out of date Unless my eyes deceive me. My telescope Has dashed your hope; Your tenets are refuted. Let me be terse:
More informationSolar System Fundamentals. What is a Planet? Planetary orbits Planetary temperatures Planetary Atmospheres Origin of the Solar System
Solar System Fundamentals What is a Planet? Planetary orbits Planetary temperatures Planetary Atmospheres Origin of the Solar System Properties of Planets What is a planet? Defined finally in August 2006!
More informationThe content is based on the National Science Teachers Association (NSTA) standards and is aligned with state standards.
Literacy Advantage Physical Science Physical Science Literacy Advantage offers a tightly focused curriculum designed to address fundamental concepts such as the nature and structure of matter, the characteristics
More informationScience In Action 8 Unit C - Light and Optical Systems. 1.1 The Challenge of light
1.1 The Challenge of light 1. Pythagoras' thoughts about light were proven wrong because it was impossible to see A. the light beams B. dark objects C. in the dark D. shiny objects 2. Sir Isaac Newton
More informationThe Solar Journey: Modeling Features of the Local Bubble and Galactic Environment of the Sun
The Solar Journey: Modeling Features of the Local Bubble and Galactic Environment of the Sun P.C. Frisch and A.J. Hanson Department of Astronomy and Astrophysics University of Chicago and Computer Science
More informationObserving the Sun NEVER LOOK DIRECTLY AT THE SUN!!! Image taken from the SOHO web-site http://sohowww.nascom.nasa.gov/gallery/solarcorona/uvc003.
name Observing the Sun NEVER LOOK DRECTLY AT THE SUN!!! mage taken from the SOHO web-site http://sohowww.nascom.nasa.gov/gallery/solarcorona/uvc003.html Explanation: The Sun is a pretty active star. You
More informationA short history of telescopes and astronomy: Galileo to the TMT
A short history of telescopes and astronomy: Galileo to the TMT Telescopes in the last 400 years Galileo 1608 Hans Lippershey applied for a patent for seeing things far away as if they were nearby 1609
More informationThe Universe. The Solar system, Stars and Galaxies
The Universe The Universe is everything. All us, the room, the U.S. the earth, the solar system, all the other stars in the Milky way galaxy, all the other galaxies... everything. How big and how old is
More information