Astronomy 103 Final Review. Spring 2009
|
|
|
- Hubert Goodman
- 6 years ago
- Views:
Transcription
1 Astronomy 103 Final Review Spring 2009
2 What aspect of Sagi>arius A* shows evidence of a massive black hole in the center of our Galaxy? A. It is emiing considerable 21 cm radiakon. B. It has ejected a cloud of low density dust. C. It is emiing far infrared radiakon. D. Rapidly moving stars are near it.
3 What aspect of Sagi>arius A* shows evidence of a massive black hole in the center of our Galaxy? A. It is emiing considerable 21 cm radiakon. B. It has ejected a cloud of low density dust. C. It is emiing far infrared radiakon. D. Rapidly moving stars are near it.
4 Standard candles, which are essenkal tools for measuring distances to remote galaxies, are A. stars and other objects of known intrinsic brightness whose apparent brightness can then be used to find the distance. B. standard laboratory light sources with which the brightness of a galaxy can be compared. C. heat sources of standard intensity used to calibrate infrared observakons of galaxies. D. laboratory light sources with accurately measured spectra for calibrakng stellar and galackc spectra.
5 Standard candles, which are essenkal tools for measuring distances to remote galaxies, are A. stars and other objects of known intrinsic brightness whose apparent brightness can then be used to find the distance. B. standard laboratory light sources with which the brightness of a galaxy can be compared. C. heat sources of standard intensity used to calibrate infrared observakons of galaxies. D. laboratory light sources with accurately measured spectra for calibrakng stellar and galackc spectra.
6 The Hubble law says that if galaxy B has twice the redshiv of galaxy A, then galaxy B is A. half as distant as galaxy A. B. twice as distant as galaxy A. C. half as hot as galaxy A. D. twice as hot as galaxy A.
7 The Hubble law says that if galaxy B has twice the redshiv of galaxy A, then galaxy B is A. half as distant as galaxy A. B. twice as distant as galaxy A. C. half as hot as galaxy A. D. twice as hot as galaxy A.
8 The large scale structure of the universe shows us that A. Visible ma>er formed along dark ma>er filaments B. Superclusters are ulkmately the result of density fluctuakons in the early universe C. Voids in the universe get larger with Kme D. All of the above
9 The large scale structure of the universe shows us that A. Visible ma>er formed along dark ma>er filaments B. Superclusters are ulkmately the result of density fluctuakons in the early universe C. Voids in the universe get larger with Kme D. All of the above
10 The era of recombinakon (380,000 years aver the Big Bang) is when A. Pop III stars began to form B. The first atoms formed C. Neutrinos could freely travel into space D. The universe began its inflakon phase
11 The era of recombinakon (380,000 years aver the Big Bang) is when A. Pop III stars began to form B. The first atoms formed C. Neutrinos could freely travel into space D. The universe began its inflakon phase
12 The rotakon curve for spiral galaxies remains remarkably constant at large distances from the central bulge. What is the significance? A. These galaxies contain significant amounts of dark ma>er that cannot be detected using electromagnekc radiakon at any wavelength. B. The stars in these galaxies, like planets orbikng the Sun in our own solar system, move primarily under the gravitakonal pull of a large mass at the center of the system. C. The stars in these galaxies influence each other gravitakonally in such a way that the galaxy rotates like a solid disk. D. Most of the mass of these galaxies is located in the disk; relakvely li>le mass is located in the central bulge.
13 The rotakon curve for spiral galaxies remains remarkably constant at large distances from the central bulge. What is the significance? A. These galaxies contain significant amounts of dark ma>er that cannot be detected using electromagnekc radiakon at any wavelength. B. The stars in these galaxies, like planets orbikng the Sun in our own solar system, move primarily under the gravitakonal pull of a large mass at the center of the system. C. The stars in these galaxies influence each other gravitakonally in such a way that the galaxy rotates like a solid disk. D. Most of the mass of these galaxies is located in the disk; relakvely li>le mass is located in the central bulge.
14 A barred spiral galaxy is a(n) A. spiral galaxy which, because of the gravitakonal influence of a neighboring galaxy, is unable to conknue, or is barred from, rotakng in a normal manner. B. spiral galaxy that has lost all its interstellar gas and dust and now just shows a central bulge crossed by a straight, featureless disk. C. galaxy with a straight bar of stars passing through its nucleus and spiral arms extending from the ends of the bar. D. edge on galaxy with a very dense dust lane in its plane that blocks light from the spiral arms and disk.
15 A barred spiral galaxy is a(n) A. spiral galaxy which, because of the gravitakonal influence of a neighboring galaxy, is unable to conknue, or is barred from, rotakng in a normal manner. B. spiral galaxy that has lost all its interstellar gas and dust and now just shows a central bulge crossed by a straight, featureless disk. C. galaxy with a straight bar of stars passing through its nucleus and spiral arms extending from the ends of the bar. D. edge on galaxy with a very dense dust lane in its plane that blocks light from the spiral arms and disk.
16 Which of the following is not a characteriskc of quasars? A. They have broad emission lines. B. They are less common in the early universe than they are today. C. They are at enormous distances from Earth. D. They oven give off strong radio radiakon.
17 Which of the following is not a characteriskc of quasars? A. They have broad emission lines. B. They are less common in the early universe than they are today. C. They are at enormous distances from Earth. D. They oven give off strong radio radiakon.
18 The Kdal streams appearing to come off of the Large and Small Magellenic Clouds show that A. The LMC and SMC used to be part of the Milky Way B. The gravity from the Milky Way is disrupkng the LMC and SMC as they orbit the galaxy C. The LMC and SMC are skll forming from material surrounding the Milky Way D. The Kdal streams aren t directly correlated to the LMC and SMC
19 The Kdal streams appearing to come off of the Large and Small Magellenic Clouds show that A. The LMC and SMC used to be part of the Milky Way B. The gravity from the Milky Way is disrupkng the LMC and SMC as they orbit the galaxy C. The LMC and SMC are skll forming from material surrounding the Milky Way D. The Kdal streams aren t directly correlated to the LMC and SMC
20 Radio galaxies are probably quasars A. seen face on to the accrekon disk. B. seen at an angle around 45 to the accrekon disk. C. that have run out of fuel in their accrekon disk D. that are just starkng up.
21 Radio galaxies are probably quasars A. seen face on to the accrekon disk. B. seen at an angle around 45 to the accrekon disk. C. that have run out of fuel in their accrekon disk D. that are just starkng up.
22
23 The light from more distant galaxies is more redshived because A. the photons slow down due to traveling through an expanding universe. B. more distant galaxies are traveling away faster through space. C. there is more absorbing ma>er between us and more distant galaxies. D. there was a stronger gravitakonal redshiv when the universe was younger and denser.
24 The light from more distant galaxies is more redshived because A. the photons slow down due to traveling through an expanding universe. B. more distant galaxies are traveling away faster through space. C. there is more absorbing ma>er between us and more distant galaxies. D. there was a stronger gravitakonal redshiv when the universe was younger and denser.
25 What is the significance of the cosmic microwave background radiakon discovered by Penzias and Wilson in 1964? A. It was the first radio transmission believed to indicate the presence of extraterrestrial life in the universe. B. It indicated the difference between Type I and Type II Cepheid variable stars. C. It showed a conneckon between millisecond pulsars and X ray bursters. D. It is the remnant of a burst of radiakon released during the very early history of the universe.
26 What is the significance of the cosmic microwave background radiakon discovered by Penzias and Wilson in 1964? A. It was the first radio transmission believed to indicate the presence of extraterrestrial life in the universe. B. It indicated the difference between Type I and Type II Cepheid variable stars. C. It showed a conneckon between millisecond pulsars and X ray bursters. D. It is the remnant of a burst of radiakon released during the very early history of the universe.
27 If the universe is closed, then parallel lines A. will remain parallel no ma>er how far they extend. B. will diverge away from each other as they extend into space. C. will eventually come together and intersect as they extend into space. D. are undefined.
28 If the universe is closed, then parallel lines A. will remain parallel no ma>er how far they extend. B. will diverge away from each other as they extend into space. C. will eventually come together and intersect as they extend into space. D. are undefined.
29 Most of the light from a spiral galaxy comes from the central bulge, so most of the mass of the galaxy resides in the central bulge. How then would we expect the rotakon speed to behave in the galaxy's disk? A. The rotakon speed should decrease smoothly with increasing distance from the center because of Kepler's law. B. The rotakon speed should increase smoothly with increasing distance from the center. C. The rotakon speed should decrease rapidly to zero just outside the central bulge because the disk has such a low mass compared to the bulge. D. The rotakon speed should remain essenkally constant with increasing distance from the center because the bulge is an extended mass, not a point mass.
30 Most of the light from a spiral galaxy comes from the central bulge, so most of the mass of the galaxy resides in the central bulge. How then would we expect the rotakon speed to behave in the galaxy's disk? A. The rotakon speed should decrease smoothly with increasing distance from the center because of Kepler's law. B. The rotakon speed should increase smoothly with increasing distance from the center. C. The rotakon speed should decrease rapidly to zero just outside the central bulge because the disk has such a low mass compared to the bulge. D. The rotakon speed should remain essenkally constant with increasing distance from the center because the bulge is an extended mass, not a point mass.
31 The most important parameter that determines the geometry of the universe is A. Age B. Density C. ComposiKon D. Temperature
32 The most important parameter that determines the geometry of the universe is A. Age B. Density C. ComposiKon D. Temperature
33 The key piece of evidence showing that the expansion of the universe is accelerakng is that the A. most distant Type Ia supernovae are fainter than they would be if the expansion were not accelerakng. B. most distant quasars are fainter than they would be if the expansion were not accelerakng. C. cosmological redshiv of light from the most distant quasars is greater than it would be if the expansion were not accelerakng. D. most distant gravitakonal lenses are weaker than they would be if the expansion were not accelerakng.
34 The key piece of evidence showing that the expansion of the universe is accelerakng is that the A. most distant Type Ia supernovae are fainter than they would be if the expansion were not accelerakng. B. most distant quasars are fainter than they would be if the expansion were not accelerakng. C. cosmological redshiv of light from the most distant quasars is greater than it would be if the expansion were not accelerakng. D. most distant gravitakonal lenses are weaker than they would be if the expansion were not accelerakng.
35 The inflakon period of the universe that occurred s aver the Big Bang can explain what phenomena? A. The homogeneity of the Cosmic Microwave Background B. The existence of dark ma>er in galaxy clusters C. The flat geometry of the universe D. Both A and C
36 The inflakon period of the universe that occurred s aver the Big Bang can explain what phenomena? A. The homogeneity of the Cosmic Microwave Background B. The existence of dark ma>er in galaxy clusters C. The flat geometry of the universe D. Both A and C
37 Cosmology is the study of A. distant quasars B. galaxy clusters C. the nature of the universe D. dark ma>er
38 Cosmology is the study of A. distant quasars B. galaxy clusters C. the nature of the universe D. dark ma>er
39 Edwin Hubble determined that the Andromeda Galaxy was a star system in its own right outside the Milky Way by studying A. X ray emission. B. globular clusters. C. molecular clouds. D. Cepheid variables.
40 Edwin Hubble determined that the Andromeda Galaxy was a star system in its own right outside the Milky Way by studying A. X ray emission. B. globular clusters. C. molecular clouds. D. Cepheid variables.
41 The existence of hot, intracluster gas in galaxy clusters that emits x rays is due to A. The large amount of dark ma>er in the cluster B. Violent interackons between galaxies that strip out gas and dust C. Residual heat from the Big Bang D. Large ellipkcals that dominate the cluster center
42 The existence of hot, intracluster gas in galaxy clusters that emits x rays is due to A. The large amount of dark ma>er in the cluster B. Violent interackons between galaxies that strip out gas and dust C. Residual heat from the Big Bang D. Large ellipkcals that dominate the cluster center
43 Which of the following list (in order) the methods of measuring distances to galaxies from the closest to the farthest? A. RedshiV, Cepheid variables, Type Ia supernovae B. Cepheid variables, Type Ia supernovae, redshiv C. Type Ia supernovae, redshiv, Cepheid variables D. All methods work at all distances
44 Which of the following list (in order) the methods of measuring distances to galaxies from the closest to the farthest? A. RedshiV, Cepheid variables, Type Ia supernovae B. Cepheid variables, Type Ia supernovae, redshiv C. Type Ia supernovae, redshiv, Cepheid variables D. All methods work at all distances
45 Completely mapping the Milky Way is difficult because A. Neutral hydrogen doesn t correlate with the structure of the Milky Way B. Dust and gas block our view through the galaxy C. We don t have radio telescopes strong enough to observe structure on the opposite side of the disk D. All of the above
46 Completely mapping the Milky Way is difficult because A. Neutral hydrogen doesn t correlate with the structure of the Milky Way B. Dust and gas block our view through the galaxy C. We don t have radio telescopes strong enough to observe structure on the opposite side of the disk D. All of the above
47 The Hubble Sequence organizes galaxies according to: A. Their evolukonary stage, with galaxies moving through the Hubble Sequence as they age B. Their mass C. The apparent shape of the galaxy as viewed from Earth D. Their overall luminosity
48 The Hubble Sequence organizes galaxies according to: A. Their evolukonary stage, with galaxies moving through the Hubble Sequence as they age B. Their mass C. The apparent shape of the galaxy as viewed from Earth D. Their overall luminosity
49 Studying the posikons of superclusters throughout the universe shows that A. The universe is homogenous B. Groups of clusters are gravitakonally bound to one another to create structures like the Great A>ractor C. Clusters form along filamentary structures of dark ma>er D. The universe becomes more densely packed with galaxies as you look back in Kme
50 Studying the posikons of superclusters throughout the universe shows that A. The universe is homogenous B. Groups of clusters are gravitakonally bound to one another to create structures like the Great A>ractor C. Clusters form along filamentary structures of dark ma>er D. The universe becomes more densely packed with galaxies as you look back in Kme
51 High redshiv galaxy surveys show that: A. Galaxy structure has remained the same through the history of the universe B. Galaxies at large redshiv are similar in shape but much more massive C. Most galaxies at large redshiv are irregular D. Most galaxies at large redshiv are spiral galaxies
52 High redshiv galaxy surveys show that: A. Galaxy structure has remained the same through the history of the universe B. Galaxies at large redshiv are similar in shape but much more massive C. Most galaxies at large redshiv are irregular D. Most galaxies at large redshiv are spiral galaxies
BROCK UNIVERSITY. Test 2, March 2015 Number of pages: 9 Course: ASTR 1P02 Number of Students: 420 Date of Examination: March 5, 2015
BROCK UNIVERSITY Page 1 of 9 Test 2, March 2015 Number of pages: 9 Course: ASTR 1P02 Number of Students: 420 Date of Examination: March 5, 2015 Number of hours: 50 min Time of Examination: 18:00 18:50
Question 1. Question 2. Correct. Chapter 16 Homework. Part A
Chapter 16 Homework Due: 11:59pm on Thursday, November 17, 2016 To understand how points are awarded, read the Grading Policy for this assignment. Question 1 Following are a number of distinguishing characteristics
Chapter 19 Galaxies. Hubble Ultra Deep Field: Each dot is a galaxy of stars. More distant, further into the past. halo
Chapter 19 Galaxies Hubble Ultra Deep Field: Each dot is a galaxy of stars. More distant, further into the past halo disk bulge Barred Spiral Galaxy: Has a bar of stars across the bulge Spiral Galaxy 1
Astronomy Hour Exam 2 March 10, 2011 QUESTION 1: The half-life of Ra 226 (radium) is 1600 years. If you started with a sample of 100 Ra 226
Astronomy 101.003 Hour Exam 2 March 10, 2011 QUESTION 1: The half-life of Ra 226 (radium) is 1600 years. If you started with a sample of 100 Ra 226 atoms, approximately how many Ra 226 atoms would be left
Chapter 23 The Milky Way Galaxy Pearson Education, Inc.
Chapter 23 The Milky Way Galaxy The Milky Way is our own galaxy viewed from the inside. It is a vast collection of more than 200 billion stars, planets, nebulae, clusters, dust and gas. Our own sun and
BROCK UNIVERSITY. Test 2: June 2016 Number of pages: 10 Course: ASTR 1P02, Section 2 Number of students: 359
BROCK UNIVERSITY Page 1 of 10 Test 2: June 2016 Number of pages: 10 Course: ASTR 1P02, Section 2 Number of students: 359 Examination date: 25 June 2016 Time limit: 50 min Time of Examination: 13:00 13:50
Star systems like our Milky Way. Galaxies
Galaxies Star systems like our Milky Way Galaxies Contain a few thousand to tens of billions of stars,as well as varying amounts of gas and dust Large variety of shapes and sizes Gas and Dust in
Name Date Period. 10. convection zone 11. radiation zone 12. core
240 points CHAPTER 29 STARS SECTION 29.1 The Sun (40 points this page) In your textbook, read about the properties of the Sun and the Sun s atmosphere. Use each of the terms below just once to complete
The Universe. But first, let s talk about light! 2012 Pearson Education, Inc.
The Universe But first, let s talk about light! Light is fast! The study of light All forms of radiation travel at 300,000,000 meters (186,000 miles) per second Since objects in space are so far away,
Lecture Outlines. Chapter 23. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 23 Astronomy Today 8th Edition Chaisson/McMillan Chapter 23 The Milky Way Galaxy Units of Chapter 23 23.1 Our Parent Galaxy 23.2 Measuring the Milky Way Discovery 23-1 Early Computers
Galaxies & Introduction to Cosmology
Galaxies & Introduction to Cosmology Other Galaxies: How many are there? Hubble Deep Field Project 100 hour exposures over 10 days Covered an area of the sky about 1/100 the size of the full moon Probably
LESSON 1. Solar System
Astronomy Notes LESSON 1 Solar System 11.1 Structure of the Solar System axis of rotation period of rotation period of revolution ellipse astronomical unit What is the solar system? 11.1 Structure of the
Exam 3 Astronomy 100, Section 3. Some Equations You Might Need
Exam 3 Astronomy 100, Section 3 Some Equations You Might Need modified Kepler s law: M = [a(au)]3 [p(yr)] (a is radius of the orbit, p is the rotation period. You 2 should also remember that the period
2. Can observe radio waves from the nucleus see a strong radio source there Sagittarius A* or Sgr A*.
7/7 The Nucleus of the MW its center 1. Can t see the nucleus in visible light too much stuff in the way. 2. Can observe radio waves from the nucleus see a strong radio source there Sagittarius A* or Sgr
What is the solar system?
Notes Astronomy What is the solar system? 11.1 Structure of the Solar System Our solar system includes planets and dwarf planets, their moons, a star called the Sun, asteroids and comets. Planets, dwarf
Chapter 30. Galaxies and the Universe. Chapter 30:
Chapter 30 Galaxies and the Universe Chapter 30: Galaxies and the Universe Chapter 30.1: Stars with varying light output allowed astronomers to map the Milky Way, which has a halo, spiral arm, and a massive
The Cosmological Redshift. Cepheid Variables. Hubble s Diagram
SOME NEGATIVE EFFECTS OF THE EXPANSION OF THE UNIVERSE. Lecture 22 Hubble s Law and the Large Scale Structure of the Universe PRS: According to modern ideas and observations, what can be said about the
Chapter 15 The Milky Way Galaxy. The Milky Way
Chapter 15 The Milky Way Galaxy The Milky Way Almost everything we see in the night sky belongs to the Milky Way We see most of the Milky Way as a faint band of light across the sky From the outside, our
Physics HW Set 3 Spring 2015
1) If the Sun were replaced by a one solar mass black hole 1) A) life here would be unchanged. B) we would still orbit it in a period of one year. C) all terrestrial planets would fall in immediately.
Chapter 15 Galaxies and the Foundation of Modern Cosmology
15.1 Islands of stars Chapter 15 Galaxies and the Foundation of Modern Cosmology Cosmology: study of galaxies What are they 3 major types of galaxies? Spiral galaxies: like the milky way, look like flat,
The King's University College Astronomy 201 Mid-Term Exam Solutions
The King's University College Astronomy 201 Mid-Term Exam Solutions Instructions: The exam consists of two sections. Part A is 20 multiple choice questions - please record answers on the sheet provided.
M31 - Andromeda Galaxy M110 M32
UNIT 4 - Galaxies XIV. The Milky Way galaxy - a huge collection of millions or billions of stars, gas, and dust, isolated in space and held together by its own gravity M110 M31 - Andromeda Galaxy A. Structure
Beyond Our Solar System Chapter 24
Beyond Our Solar System Chapter 24 PROPERTIES OF STARS Distance Measuring a star's distance can be very difficult Stellar parallax Used for measuring distance to a star Apparent shift in a star's position
Astronomy 113. Dr. Joseph E. Pesce, Ph.D. Review. Semester Recap. Nature of Light. Wavelength. Red/Blue Light 4/30/18
https://www.theverge.com/2018/ 3/10/17104188/melodysheeptime-lapse-universe-earthformation-watch Astronomy 113 Dr. Joseph E. Pesce, Ph.D. Review Semester Recap ³Light and Radiation ³The Sun ³Measuring
The Milky Way Galaxy. Some thoughts. How big is it? What does it look like? How did it end up this way? What is it made up of?
Some thoughts The Milky Way Galaxy How big is it? What does it look like? How did it end up this way? What is it made up of? Does it change 2 3 4 5 This is not a constant zoom The Milky Way Almost everything
Chapter 23: Dark Matter, Dark Energy & Future of the Universe. Galactic rotation curves
Chapter 23: Dark Matter, Dark Energy & Future of the Universe Galactic rotation curves Orbital speed as a function of distance from the center: rotation_of_spiral_galaxy.htm Use Kepler s Third Law to get
ASTR 1P02 Test 2, March 2017 Page 1 BROCK UNIVERSITY. Test 2: March 2017 Number of pages: 9 Course: ASTR 1P02, Section 2 Number of students: 1193
ASTR 1P02 Test 2, March 2017 Page 1 BROCK UNIVERSITY Test 2: March 2017 Number of pages: 9 Course: ASTR 1P02, Section 2 Number of students: 1193 Examination date: 4 March 2017 Time limit: 50 min Time of
Lecture Outlines. Chapter 24. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 24 Astronomy Today 8th Edition Chaisson/McMillan Chapter 24 Galaxies Units of Chapter 24 24.1 Hubble s Galaxy Classification 24.2 The Distribution of Galaxies in Space 24.3 Hubble
BROCK UNIVERSITY. Test 2, March 2018 Number of pages: 9 Course: ASTR 1P02, Section 1 Number of Students: 465 Date of Examination: March 12, 2018
BROCK UNIVERSITY Page 1 of 9 Test 2, March 2018 Number of pages: 9 Course: ASTR 1P02, Section 1 Number of Students: 465 Date of Examination: March 12, 2018 Number of hours: 50 min Time of Examination:
Homework 6 Name: Due Date: June 9, 2008
Homework 6 Name: Due Date: June 9, 2008 1. Where in the universe does the general expansion occur? A) everywhere in the universe, including our local space upon Earth, the solar system, our galaxy and
Chapter 15 2/19/2014. Lecture Outline Hubble s Galaxy Classification. Normal and Active Galaxies Hubble s Galaxy Classification
Lecture Outline Chapter 15 Normal and Active Galaxies Spiral galaxies are classified according to the size of their central bulge. Chapter 15 Normal and Active Galaxies Type Sa has the largest central
Exam 4 Review EXAM COVERS LECTURES 22-29
Exam 4 Review EXAM COVERS LECTURES 22-29 Theoretically is there a center of the universe? Is there an edge? Do we know where Earth is on this? There is no center to the Universe, What kind of light we
8/30/2010. Classifying Stars. Classifying Stars. Classifying Stars
Classifying Stars In the early 1900s, Ejnar Hertzsprung and Henry Russell made some important observations. They noticed that, in general, stars with higher temperatures also have brighter absolute magnitudes.
Prentice Hall EARTH SCIENCE
Prentice Hall EARTH SCIENCE Tarbuck Lutgens Chapter 25 Beyond Our Solar System 25.1 Properties of Stars Characteristics of Stars A constellation is an apparent group of stars originally named for mythical
Island Universes. Up to 1920 s, many thought that Milky Way encompassed entire universe.
Island Universes Up to 1920 s, many thought that Milky Way encompassed entire universe. Observed three types of nebulas (clouds): - diffuse, spiral, elliptical - many were faint, indistinct - originally
According to the currents models of stellar life cycle, our sun will eventually become a. Chapter 34: Cosmology. Cosmology: How the Universe Works
Chapter 34: Cosmology According to the currents models of stellar life cycle, our sun will eventually become a a) Cloud of hydrogen gas b) Protostar c) Neutron star d) Black hole e) White dwarf id you
It is about 100,000 ly across, 2,000 ly thick, and our solar system is located 26,000 ly away from the center of the galaxy.
The Galaxies The Milky Way Galaxy Is a spiral galaxy in which our solar system is located. The center of the galaxy lies in the Sagittarius Constellation. It is about 100,000 ly across, 2,000 ly thick,
29:50 Stars, Galaxies, and the Universe Final Exam December 13, 2010 Form A
29:50 Stars, Galaxies, and the Universe Final Exam December 13, 2010 Form A There are 40 questions. Read each question and all of the choices before choosing. Budget your time. No whining. Walk with Ursus!
(Astronomy for Dummies) remark : apparently I spent more than 1 hr giving this lecture
(Astronomy for Dummies) remark : apparently I spent more than 1 hr giving this lecture A.D. 125? Ptolemy s geocentric model Planets ( ) wander among stars ( ) For more info: http://aeea.nmns.edu.tw/aeea/contents_list/universe_concepts.html
Cosmology, Galaxies, and Stars OUR VISIBLE UNIVERSE
Cosmology, Galaxies, and Stars OUR VISIBLE UNIVERSE Cosmology Cosmology is the study of the universe; its nature, origin and evolution. General Relativity is the mathematical basis of cosmology from which
The Milky Way. Mass of the Galaxy, Part 2. Mass of the Galaxy, Part 1. Phys1403 Stars and Galaxies Instructor: Dr. Goderya
Foundations Chapter of Astronomy 15 13e Our Milky Way Seeds Phys1403 Stars and Galaxies Instructor: Dr. Goderya Selected Topics in Chapter 15 A view our Milky Way? The Size of our Milky Way The Mass of
25.2 Stellar Evolution. By studying stars of different ages, astronomers have been able to piece together the evolution of a star.
25.2 Stellar Evolution By studying stars of different ages, astronomers have been able to piece together the evolution of a star. Star Birth The birthplaces of stars are dark, cool interstellar clouds,
View of the Galaxy from within. Lecture 12: Galaxies. Comparison to an external disk galaxy. Where do we lie in our Galaxy?
Lecture 12: Galaxies View of the Galaxy from within The Milky Way galaxy Rotation curves and dark matter External galaxies and the Hubble classification scheme Plotting the sky brightness in galactic coordinates,
Astronomy 113. Dr. Joseph E. Pesce, Ph.D. Distances & the Milky Way. The Curtis View. Our Galaxy. The Shapley View 3/27/18
Astronomy 113 Dr. Joseph E. Pesce, Ph.D. Distances & the Milky Way 14-2 Historical Overview: the Curtis-Shapley Debate ³What is the size of our galaxy? ³What is the nature of spiral nebula? The Curtis
Astronomy 113. Dr. Joseph E. Pesce, Ph.D. Dr. Joseph E. Pesce, Ph.D.
Astronomy 113 Dr. Joseph E. Pesce, Ph.D. Distances & the Milky Way Historical Overview: the Curtis-Shapley Debate ³What is the size of our galaxy? ³What is the nature of spiral nebula? 14-2 ³Occurred in
Energy Source for Active Galactic Nuclei
Quasars Quasars are small, extremely luminous, extremely distant galactic nuclei Bright radio sources Name comes from Quasi-Stellar Radio Source, as they appeared to be stars! Can have clouds of gas near
Active Galaxies and Galactic Structure Lecture 22 April 18th
Active Galaxies and Galactic Structure Lecture 22 April 18th FINAL Wednesday 5/9/2018 6-8 pm 100 questions, with ~20-30% based on material covered since test 3. Do not miss the final! Extra Credit: Thursday
Our Galaxy. Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust. Held together by gravity! The Milky Way with the Naked Eye
Our Galaxy Milky Way Galaxy = Sun + ~100 billion other stars + gas and dust Held together by gravity! The Milky Way with the Naked Eye We get a special view of our own galaxy because we are part of it!
Neutron Stars. Neutron Stars and Black Holes. The Crab Pulsar. Discovery of Pulsars. The Crab Pulsar. Light curves of the Crab Pulsar.
Chapter 11: Neutron Stars and Black Holes A supernova explosion of an M > 8 M sun star blows away its outer layers. Neutron Stars The central core will collapse into a compact object of ~ a few M sun.
Reminders! Observing Projects: Both due Monday. They will NOT be accepted late!!!
Reminders! Website: http://starsarestellar.blogspot.com/ Lectures 1-15 are available for download as study aids. Reading: You should have Chapters 1-14 read. Read Chapters 15-17 by the end of the week.
Big Galaxies Are Rare! Cepheid Distance Measurement. Clusters of Galaxies. The Nature of Galaxies
Big Galaxies Are Rare! Potato Chip Rule: More small things than large things Big, bright spirals are easy to see, but least common Dwarf ellipticals & irregulars are most common Faint, hard to see Mostly
The Contents of the Universe (or/ what do we mean by dark matter and dark energy?)
The Contents of the Universe (or/ what do we mean by dark matter and dark energy?) Unseen Influences Dark Matter: An undetected form of mass that emits little or no light but whose existence we infer from
Figure 19.19: HST photo called Hubble Deep Field.
19.3 Galaxies and the Universe Early civilizations thought that Earth was the center of the universe. In the sixteenth century, we became aware that Earth is a small planet orbiting a medium-sized star.
Earth Science, 13e Tarbuck & Lutgens
Earth Science, 13e Tarbuck & Lutgens Beyond Our Solar System Earth Science, 13e Chapter 24 Stanley C. Hatfield Southwestern Illinois College Properties of stars Distance Distances to the stars are very
GraspIT Questions AQA GCSE Physics Space physics
A. Solar system: stability of orbital motions; satellites (physics only) 1. Put these astronomical objects in order of size from largest to smallest. (3) Fill in the boxes in the correct order. the Moon
THE UNIVERSE CHAPTER 20
THE UNIVERSE CHAPTER 20 THE UNIVERSE UNIVERSE everything physical in and Includes all space, matter, and energy that has existed, now exists, and will exist in the future. How did our universe form, how
A 103 Notes, Week 14, Kaufmann-Comins Chapter 15
NEARBY GALAXIES I. Brief History A 103 Notes, Week 14, Kaufmann-Comins Chapter 15 A. Kant B. Curtis-Shapley debate C. Distance to Andromeda II. Classification of nearby galaxies: Spirals, Ellipticals,
AS1001: Galaxies and Cosmology
AS1001: Galaxies and Cosmology Keith Horne kdh1@st-and.ac.uk http://www-star.st-and.ac.uk/~kdh1/eg/eg.html Text: Kutner Astronomy:A Physical Perspective Chapters 17-21 Cosmology Today Blah Title Current
BROCK UNIVERSITY. Test 2: July 2015 Number of pages: 9 Course: ASTR 1P02, Section 2 Number of students: 318
BROCK UNIVERSITY Page 1 of 9 Test 2: July 2015 Number of pages: 9 Course: ASTR 1P02, Section 2 Number of students: 318 Examination date: 4 July 2015 Time limit: 50 min Time of Examination: 13:00 13:50
Stars and Galaxies 1
Stars and Galaxies 1 Characteristics of Stars 2 Star - body of gases that gives off great amounts of radiant energy as light and heat 3 Most stars look white but are actually different colors Antares -
Learning Objectives: Chapter 13, Part 1: Lower Main Sequence Stars. AST 2010: Chapter 13. AST 2010 Descriptive Astronomy
Chapter 13, Part 1: Lower Main Sequence Stars Define red dwarf, and describe the internal dynamics and later evolution of these low-mass stars. Appreciate the time scale of late-stage stellar evolution
Part two of a year-long introduction to astrophysics:
ASTR 3830 Astrophysics 2 - Galactic and Extragalactic Phil Armitage office: JILA tower A909 email: pja@jilau1.colorado.edu Spitzer Space telescope image of M81 Part two of a year-long introduction to astrophysics:
Lecture 32: The Expanding Universe Readings: Sections 26-5 and 28-2
Lecture 32: The Expanding Universe Readings: Sections 26-5 and 28-2 Key Ideas Measuring the Distances to Galaxies and Determining the Scale of the Universe Distance Methods: Trigonometric Parallaxes Spectroscopic
Number of Stars: 100 billion (10 11 ) Mass : 5 x Solar masses. Size of Disk: 100,000 Light Years (30 kpc)
THE MILKY WAY GALAXY Type: Spiral galaxy composed of a highly flattened disk and a central elliptical bulge. The disk is about 100,000 light years (30kpc) in diameter. The term spiral arises from the external
Galaxies with Active Nuclei. Active Galactic Nuclei Seyfert Galaxies Radio Galaxies Quasars Supermassive Black Holes
Galaxies with Active Nuclei Active Galactic Nuclei Seyfert Galaxies Radio Galaxies Quasars Supermassive Black Holes Active Galactic Nuclei About 20 25% of galaxies do not fit well into Hubble categories
Our View of the Milky Way. 23. The Milky Way Galaxy
23. The Milky Way Galaxy The Sun s location in the Milky Way galaxy Nonvisible Milky Way galaxy observations The Milky Way has spiral arms Dark matter in the Milky Way galaxy Density waves produce spiral
A100H Exploring the Universe: Quasars, Dark Matter, Dark Energy. Martin D. Weinberg UMass Astronomy
A100H Exploring the :, Dark Matter, Dark Energy Martin D. Weinberg UMass Astronomy astron100h-mdw@courses.umass.edu April 19, 2016 Read: Chaps 20, 21 04/19/16 slide 1 BH in Final Exam: Friday 29 Apr at
Lecture 14: Other Galaxies A2020 Prof. Tom Megeath. The Milky Way in the Infrared 3/17/10. NGC 7331: the Milky Way s Twins. Spiral Galaxy bulge halo
Lecture 14: Other Galaxies A2020 Prof. Tom Megeath Our Galaxy: Side View We see our galaxy edge-on Primary features: Disk: young and old stars where we live. Bulge: older stars Halo: oldest stars, globular
Astronomy A BEGINNER S GUIDE TO THE UNIVERSE EIGHTH EDITION
Astronomy A BEGINNER S GUIDE TO THE UNIVERSE EIGHTH EDITION CHAPTER 14 The Milky Way Galaxy Lecture Presentation 14.0 the Milky Way galaxy How do we know the Milky Way exists? We can see it even though
Galaxies Guiding Questions
Galaxies Guiding Questions How did astronomers first discover other galaxies? How did astronomers first determine the distances to galaxies? Do all galaxies have spiral arms, like the Milky Way? How do
Galaxies and the expansion of the Universe
Review of Chapters 14, 15, 16 Galaxies and the expansion of the Universe 5/4/2009 Habbal Astro 110-01 Review Lecture 36 1 Recap: Learning from Light How does light tell us what things are made of? Every
Normal Galaxies (Ch. 24) + Galaxies and Dark Matter (Ch. 25) Symbolically: E0.E7.. S0..Sa..Sb..Sc..Sd..Irr
Normal Galaxies (Ch. 24) + Galaxies and Dark Matter (Ch. 25) Here we will cover topics in Ch. 24 up to 24.4, but then skip 24.4, 24.5 and proceed to 25.1, 25.2, 25.3. Then, if there is time remaining,
Review of Lecture 15 3/17/10. Lecture 15: Dark Matter and the Cosmic Web (plus Gamma Ray Bursts) Prof. Tom Megeath
Lecture 15: Dark Matter and the Cosmic Web (plus Gamma Ray Bursts) Prof. Tom Megeath A2020 Disk Component: stars of all ages, many gas clouds Review of Lecture 15 Spheroidal Component: bulge & halo, old
Our Galaxy. We are located in the disk of our galaxy and this is why the disk appears as a band of stars across the sky.
Our Galaxy Our Galaxy We are located in the disk of our galaxy and this is why the disk appears as a band of stars across the sky. Early attempts to locate our solar system produced erroneous results.
The Milky Way. Finding the Center. Milky Way Composite Photo. Finding the Center. Milky Way : A band of and a. Milky Way
The Milky Way Milky Way : A band of and a The band of light we see is really 100 billion stars Milky Way probably looks like Andromeda. Milky Way Composite Photo Milky Way Before the 1920 s, astronomers
Ay162, Spring 2006 Week 8 p. 1 of 15
Astronomy 162, Week 8 Milky Way Galaxy, continued Patrick S. Osmer Spring, 2006 Rotation of Galaxy How do we know the galaxy is rotating, and how do we measure its rotation? Measure radial velocities of
Chapter 25 (and end of 24): Lecture Notes
Chapter 25 (and end of 24): Lecture Notes In order to understand the Hubble Law and its implications both for estimating distances and for interpreting the evolution of the universe, you have to be comfortable
Overview DARK MATTER & DARK ENERGY. Dark Matter and Dark Energy I. Definition Current Understanding Detection Methods Cosmological Impact
DARK MATTER & DARK ENERGY Source: Max Ehrhardt Modiefied for Astronomy 101 Dark Matter and Dark Energy I Physics 113 Goderya Chapter(s): 18 Learning Outcomes: Overview Definition Current Understanding
Notes for Wednesday, July 16; Sample questions start on page 2 7/16/2008
Notes for Wednesday, July 16; Sample questions start on page 2 7/16/2008 Wed, July 16 MW galaxy, then review. Start with ECP3Ch14 2 through 8 Then Ch23 # 8 & Ch 19 # 27 & 28 Allowed Harlow Shapely to locate
TA Final Review. Class Announcements. Objectives Today. Compare True and Apparent brightness. Finding Distances with Cepheids
Class Announcements Vocab Quiz 4 deadline is Saturday Midterm 4 has started, ends Monday Lab was in the Planetarium. You still need to do the 2 questions Check PS100 webpage, make sure your clicker is
Revision Guide for Chapter 12
Revision Guide for Chapter 12 Contents Student s Checklist Revision Notes The speed of light... 4 Doppler effect... 4 Expansion of the Universe... 5 Microwave background radiation... 5 Galaxy... 6 Summary
Final exam is Wednesday, December 14, in LR 1 VAN at 9:45 am.
Announcements Final exam is Wednesday, December 14, in LR 1 VAN at 9:45 am. Office hours: Tuesday 9-11 am, 1 2 pm, and 3-4 pm or by appointment in 702 VAN There will be no Astronomy tutorial during finals
4/6/17. SEMI-WARM stuff: dust. Tour of Galaxies. Our Schedule
ASTR 1040: Stars & Galaxies Super-bubble blowout in NGC 3709 Prof. Juri Toomre TAs: Piyush Agrawal, Connor Bice Lecture 22 Thur 6 Apr 2017 zeus.colorado.edu/astr1040-toomre Tour of Galaxies Look at complex
Chapter 28 Stars and Their Characteristics
Chapter 28 Stars and Their Characteristics Origin of the Universe Big Bang Theory about 10-20 bya all matter in the universe existed in a hot dense state about the size of an atom (tiny). That matter sort
2) On a Hertzsprung-Russell diagram, where would you find red giant stars? A) upper right B) lower right C) upper left D) lower left
Multiple choice test questions 2, Winter Semester 2015. Based on parts covered after mid term. Essentially on Ch. 12-2.3,13.1-3,14,16.1-2,17,18.1-2,4,19.5. You may use a calculator and the useful formulae
Hubble s Law. Tully-Fisher relation. The redshift. λ λ0. Are there other ways to estimate distances? Yes.
Distances to galaxies Cepheids used by Hubble, 1924 to show that spiral nebulae like M31 were further from the Sun than any part of the Milky Way, therefore galaxies in their own right. Review of Cepheids
Exam 3 Astronomy 114
Exam 3 Astronomy 114 Select the answer that is the most appropriate among the choices given. 1. What is the Hubble law? (A) a relation between a galaxy s mass and radius. (B) a rule that describes the
The Milky Way & Galaxies
The Milky Way & Galaxies The Milky Way Appears as a milky band of light across the sky A small telescope reveals that it is composed of many stars (Galileo again!) Our knowledge of the Milky Way comes
COSMOLOGY PHYS 30392 OBSERVING THE UNIVERSE Part I Giampaolo Pisano - Jodrell Bank Centre for Astrophysics The University of Manchester - January 2013 http://www.jb.man.ac.uk/~gp/ giampaolo.pisano@manchester.ac.uk
Galaxies. With a touch of cosmology
Galaxies With a touch of cosmology Types of Galaxies Spiral Elliptical Irregular Spiral Galaxies Spiral Galaxies Disk component where the spiral arms are Interstellar medium Star formation Spheroidal
CH 14 MODERN COSMOLOGY The Study of Nature, origin and evolution of the universe Does the Universe have a center and an edge? What is the evidence
CH 14 MODERN COSMOLOGY The Study of Nature, origin and evolution of the universe Does the Universe have a center and an edge? What is the evidence that the Universe began with a Big Bang? How has the Universe
24.1 Hubble s Galaxy Classification
Chapter 24 Galaxies Units of Chapter 24 24.1 Hubble s Galaxy Classification 24.2 The Distribution of Galaxies in Space 24.3 Hubble s Law 24.4 XXActive Galactic Nuclei XXRelativistic Redshifts and Look-Back
Beyond the Solar System 2006 Oct 17 Page 1 of 5
I. Stars have color, brightness, mass, temperature and size. II. Distances to stars are measured using stellar parallax a. The further away, the less offset b. Parallax angles are extremely small c. Measured
Lecture PowerPoints. Chapter 33 Physics: Principles with Applications, 7 th edition Giancoli
Lecture PowerPoints Chapter 33 Physics: Principles with Applications, 7 th edition Giancoli This work is protected by United States copyright laws and is provided solely for the use of instructors in teaching
UNIT 3 The Study of the. Universe. Chapter 7: The Night Sky. Chapter 8: Exploring Our Stellar Neighbourhood. Chapter 9:The Mysterious.
UNIT 3 The Study of the Universe Chapter 7: The Night Sky Chapter 8: Exploring Our Stellar Neighbourhood Chapter 9:The Mysterious Universe CHAPTER 9 The Mysterious Universe In this chapter, you will: identify
ASTR Final Examination Phil Armitage, Bruce Ferguson
ASTR 1120-001 Final Examination Phil Armitage, Bruce Ferguson FINAL EXAM MAY 6 th 2006: Closed books and notes, 1.5 hours. Please PRINT your name and student ID on the places provided on the scan sheet.
The Universe. is space and everything in it.
The Universe is space and everything in it. Galaxies A galaxy is a supercluster of stars, gas, and dust that are held together by gravity. There are three main types of galaxies: Irregular Elliptical Spiral
Cosmic Microwave Background Radiation
Base your answers to questions 1 and 2 on the passage below and on your knowledge of Earth Science. Cosmic Microwave Background Radiation In the 1920s, Edwin Hubble's discovery of a pattern in the red
The Milky Way Galaxy (ch. 23)
The Milky Way Galaxy (ch. 23) [Exceptions: We won t discuss sec. 23.7 (Galactic Center) much in class, but read it there will probably be a question or a few on it. In following lecture outline, numbers
Lecture 19: Galaxies. Astronomy 111
Lecture 19: Galaxies Astronomy 111 Galaxies What is a galaxy? Large assembly of stars, gas and dust, held together by gravity Sizes: Largest: ~1 Trillion stars (or more) Smallest: ~10 Million stars Milky