Revision: Sun, Stars (and Planets) See web slides of Dr Clements for Planets revision. Juliet Pickering Office: Huxley 706
|
|
|
- Daniela Horn
- 5 years ago
- Views:
Transcription
1 Revision: Sun, Stars (and Planets) See web slides of Dr Clements for Planets revision Juliet Pickering Office: Huxley 706 Office hour (Pickering): Thursday 22nd May pm
2 Outline overview of first part of the course The Sun: its structure and energy generation Stars: putting the Sun into context
3 Solar structure and energy generation: What is a star? Stellar structure equations Estimates of ρ, P, T etc energy generation nuclear burning convection vs radiation Interior structure Timescales (thermal, dynamical) Solar Atmosphere, Solar activity Solar spectrum
4 Hydrostatic equilibrium Mass continuity Energy generation
5 Equation of state You need to know this!
6 Solar atmosphere Photosphere Chromosphere Transition region Corona Solar wind Magnetic Activity
7
8 Intensity vs wavelength, Planck curves for blackbodies at a range of different temperatures Wavelength Wavelength /nm
9 Stars: putting the Sun into context White dwarfs supergiants Main sequence Red giants m1 r 1 r 2 r O m 2
10 Physical parameters and their measurement: egs L, magnitude absolute and apparent distance (parsec pc, light years, AU) parallax, proper motion effective T, colour index age radius, mass, composition (stellar spectrum, spectral type, spectral classification, opacity) Units (arc sec, parsec, light year, solar units etc)
11 Spectral classification of stars Type Colour Teff (K) Main characteristics O Blue > He+ lines; strong UV Examples Mintaka (δ Orionis) B Blue-white Neutral He lines Rigel, Spica A White Strong H lines Sirius, Vega F Yellow-white Weak metal lines Procyon G Yellow Solar-like spectrum K Orange Metal lines dominate M Red < 3500 Molecular bands noticeable Sun, Capella Arcturus, Aldebaran Betelgeuse, Antares Each class also divided into 10 subdivisions, so e.g., B8, B9, A0, A1, A2, A9, F0, F1, 0 being hottest, so F9 and G0 are very similar stars
12 HR diagram and stellar evolution dependence on stellar mass, types of stars time spent in different stages explanations Evolutionary tracks homologous series, Age of star clusters
13 HR diagrams most luminous supergiants less luminous supergiants M v luminous giants normal giants subgiants B-V O B A F G K M dwarfs (main-sequence stars) L M 4
14 supergiants Red giants Main sequence White dwarfs
15 Pleiades Homology transformation Consider set of stars of homogeneous composition, burning hydrogen. Stars differ only because of their mass. Derived many relations, egs: ρ c M / R 3 Pc M 2 / R 4 T c M / R etc etc
16 So massive stars (at top of main sequence) exhaust their hydrogen quickest -- explains turn-off point in clusters.
17 Estimating cluster age Use a relevant M-L relation: Or even simpler : see problem sheet 3 for rough estimate
18 Stellar evolutionary tracks on an HR diagram G F D H B E A C
19
20 Binary Stars -Visual -Spectroscopic -Eclipsing m 1 r 1 r 2 r O m 2
21 Revision: Sun, Stars (and Planets) See web slides of Dr Clements for Planets revision Juliet Pickering Office: Huxley 706 Office hours (Pickering): Thursday 22nd May pm
22 Good luck! Any questions?
23 Sun, Stars & Planets Revision Lecture Dave Clements & Juliet Pickering Thursday, 8 May 14
24 Overview The Exam & Exam advice Stars Summary Planets Summary Questions Thursday, 8 May 14
25 The Exam Format same as previous years: Section A: compulsory [40 marks] Will include a question on stars & a question on planets Section B Choose 2 questions out of 4 [30 marks each] Will include an essay type question Thursday, 8 May 14
26 What you are Given List of constants Equations of Stellar structure Thursday, 8 May 14
27 Fundamental physical constants a radiation density constant Jm 1 K 4 c speed of light ms 1 G Gravitational constant Nm 2 kg 2 h Planck s constant Js k Boltzmann s constant JK 1 e electron charge C m e mass of electron kg m H mass of hydrogen atom kg N A Avogadro s number mol Stefan-Boltzmann constant Wm 2 K 4 0 permittivity of free space Fm 1 µ 0 permeability of free space Hm 1 R Gas constant JK 1 kg 1 Astrophysical quantities L solar luminosity W M solar mass kg R solar radius m T eff effective temperature of Sun 5780 K AU astronomical unit m pc parsec m Thursday, 8 May 14
28 Equations of Stellar Structure dm dr = 4 r 2 dp dr = Gm r 2 dt dr = 3apple L 16 acr 2 T 3 if heat transport is radiative dt dr = 1 1! T P dp dr if heat transport is convective dl dr = 4 r 2 Thursday, 8 May 14
29 Exam Advice: 1 Read all questions before choosing which to do Read them carefully: eg. sketch does not mean plot exactly, estimate does not mean make a precise calculation Check units: astronomical units are not SI angles - arcsec vs. radians distances - m, AU, pc Thursday, 8 May 14
30 Exam Advice: 2 Remember: one answer book for each question Write legibly!!!! Give intermediate steps so we can follow what you re doing and give credit if things go wrong half way If you reach an answer you know is wrong but can t fix it, tell us it is wrong and why it is wrong Thursday, 8 May 14
31 Resources On Blackboard Lecture notes Problem sheets Handouts Slides from lectures Past papers Office hours Come and see us or us! But not at the last minute ie. weekend before the exam Thursday, 8 May 14
32 A storm on Saturn Thursday, 8 May 14
33 Solar System: Key Points Structure of the Solar System: Planets, Ecliptic, Nebular Hypothesis Kepler s Laws 1)The orbit of a planet forms an ellipse with the Sun at one focus 2)The Sun-planet vector sweeps out equal areas in equal time 3)The square of the orbital period of the planet is proportional to the cube of the orbit s semi-major axis Know & explain all 3 Show 3rd law in the context of a circular orbit Thursday, 8 May 14
34 Planets: Key Points Terrestrial Planets: atmospheric & interior structure cooling & heating shaping of surfaces no-atmosphere temperature, Greenhouse Effect & Carbon cycle Gas Giants: structure & atmospheres ring systems and moons Roche limit Asteroids, KBOs and Comets Orbital resonances & tidal locking Comet reservoirs (Oort cloud & KBOs) and implications for comets Thursday, 8 May 14
35 Exoplanets: Key Points Detection methods: astrometry transits radial velocities equations simplified version of binaries with Mp << Ms appreciate selection effects, explain quantities being measured Exoplanet characteristics not rare, systems being found, range of eccentricities, many short-period planets including hot Jupiters Possibility of life outside the Solar System Habitable zone, Drake Equation & Fermi Paradox Thursday, 8 May 14
36 Thursday, 8 May 14
HOMEWORK - Chapter 17 The Stars
Astronomy 20 HOMEWORK - Chapter 7 The Stars Use a calculator whenever necessary. For full credit, always show your work and explain how you got your answer in full, complete sentences on a separate sheet
My God, it s full of stars! AST 248
My God, it s full of stars! AST 248 N * The number of stars in the Galaxy N = N * f s f p n h f l f i f c L/T The Galaxy M31, the Andromeda Galaxy 2 million light years from Earth The Shape of the Galaxy
Astronomy 113. Dr. Joseph E. Pesce, Ph.D. Dr. Joseph E. Pesce, Ph.D.
Astronomy 113 Dr. Joseph E. Pesce, Ph.D. The Nature of Stars 8-2 Parallax For nearby stars - measure distances with parallax July 1 AU d p A A A January ³ d = 1/p (arcsec) [pc] ³ 1pc when p=1arcsec; 1pc=206,265AU=3
Types of Stars 1/31/14 O B A F G K M. 8-6 Luminosity. 8-7 Stellar Temperatures
Astronomy 113 Dr. Joseph E. Pesce, Ph.D. The Nature of Stars For nearby stars - measure distances with parallax 1 AU d p 8-2 Parallax A January ³ d = 1/p (arcsec) [pc] ³ 1pc when p=1arcsec; 1pc=206,265AU=3
Unit 16: Astronomy and space science. Learning aim A Understand the fundamental aspects of the solar system
Unit 16: Astronomy and space science Learning aim A Understand the fundamental aspects of the solar system Contents page Note: anywhere you see a capital D means you MUST draw a diagram. Radiative zone
Test #2 results. Grades posted in UNM Learn. Along with current grade in the class
Test #2 results Grades posted in UNM Learn D C B A Along with current grade in the class F Clicker Question: If the Earth had no Moon then what would happen to the tides? A: The tides would not be as strong
The Hertzprung-Russell Diagram. The Hertzprung-Russell Diagram. Question
Key Concepts: Lecture 21: Measuring the properties of stars (cont.) The Hertzsprung-Russell (HR) Diagram (L versus T) The Hertzprung-Russell Diagram The Stefan-Boltzmann Law: flux emitted by a black body
Ay 1 Midterm. Due by 5pm on Wednesday, May 9 to your head TA s mailbox (249 Cahill), or hand it directly to any section TA
Ay 1 Midterm Due by 5pm on Wednesday, May 9 to your head TA s mailbox (249 Cahill), or hand it directly to any section TA You have THREE HOURS to complete the exam, but it is about two hours long. The
MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Homework Ch 7, 8, 9 Name MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) Our most detailed knowledge of Uranus and Neptune comes from 1) A) the
OPTION E, ASTROPHYSICS TEST REVIEW
IB PHYSICS Name: DEVIL PHYSICS Period: Date: BADDEST CLASS ON CAMPUS OPTION E, ASTROPHYSICS TEST REVIEW S1. This question is about the nature of certain stars on the Hertzsprung-Russell diagram and determining
Physics 160: Stellar Astrophysics. Midterm Exam. 27 October 2011 INSTRUCTIONS READ ME!
Physics 160: Stellar Astrophysics 27 October 2011 Name: S O L U T I O N S Student ID #: INSTRUCTIONS READ ME! 1. There are 4 questions on the exam; complete at least 3 of them. 2. You have 80 minutes to
AST Section 2: Test 2
AST1002 - Section 2: Test 2 Date: 11/05/2009 Name: Equations: E = m c 2 Question 1: The Sun is a stable star because 1. gravity balances forces from pressure. (!) Miniquiz 7, Q3 2. the rate of fusion equals
OPTION E, ASTROPHYSICS TEST REVIEW
IB PHYSICS Name: DEVIL PHYSICS Period: Date: # Marks: XX Raw Score: IB Curve: BADDEST CLASS ON CAMPUS OPTION E, ASTROPHYSICS TEST REVIEW S1. This question is about the nature of certain stars on the Hertzsprung-Russell
Examination paper for FY2450 Astrophysics
1 Department of Physics Examination paper for FY2450 Astrophysics Academic contact during examination: Rob Hibbins Phone: 94820834 Examination date: 31-05-2014 Examination time: 09:00 13:00 Permitted examination
Chapter 15 Surveying the Stars
Chapter 15 Surveying the Stars 15.1 Properties of Stars Our goals for learning How do we measure stellar luminosities? How do we measure stellar temperatures? How do we measure stellar masses? How do we
Chapter 15: Surveying the Stars
Chapter 15 Lecture Chapter 15: Surveying the Stars Surveying the Stars 15.1 Properties of Stars Our goals for learning: How do we measure stellar luminosities? How do we measure stellar temperatures? How
Universe Now. 12. Revision and highlights
Universe Now 12. Revision and highlights Practical issues about the exam The exam is on Monday 6.5. (12.00-16.00), lecture hall B121 (Exactum). Paper will be provided. You have 4 hours to finish the exam,
Mass-Luminosity and Stellar Lifetimes WS
Name Mass-Luminosity and Stellar Lifetimes WS The graph shows the Mass-Luminosity Relationship for main sequence stars. Use it to answer questions 1-3. 1) A star with a mass of 0.5 solar masses would be
Chapter 15 Surveying the Stars Properties of Stars
Chapter 15 Surveying the Stars 15.1 Properties of Stars Our goals for learning: How do we measure stellar luminosities? How do we measure stellar temperatures? How do we measure stellar masses? Luminosity:
Galaxies and Stars. 3. Base your answer to the following question on The reaction below represents an energy-producing process.
Galaxies and Stars 1. To an observer on Earth, the Sun appears brighter than the star Rigel because the Sun is A) hotter than Rigel B) more luminous than Rigel C) closer than Rigel D) larger than Rigel
The Cosmic Perspective. Surveying the Properties of Stars. Surveying the Stars. How do we measure stellar luminosities?
Surveying the Stars Chapter 15 Lecture The Cosmic Perspective 15.1 Properties of Stars Our goals for learning: How do we measure stellar luminosities? How do we measure stellar temperatures? How do we
MASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Earth, Atmospheric, and Planetary Sciences Department. Quiz 2
MASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Earth, Atmospheric, and Planetary Sciences Department Astronomy 8.282J 12.402J April 13, 2005 Quiz 2 Name Last First (please print) 1. Work any
Chapter 10 Measuring the Stars
Chapter 10 Measuring the Stars Some of the topics included in this chapter Stellar parallax Distance to the stars Stellar motion Luminosity and apparent brightness of stars The magnitude scale Stellar
EVOLUTION OF STARS HERTZSPRUNG-RUSSELL DIAGRAM
VISUAL PHYSICS ONLINE EVOLUTION OF STARS HERTZSPRUNG-RUSSELL DIAGRAM The total power radiated by a star is called its intrinsic luminosity L (luminosity). The apparent brightness (apparent luminosity)
AST-1002 Section 0459 Review for Final Exam Please do not forget about doing the evaluation!
AST-1002 Section 0459 Review for Final Exam Please do not forget about doing the evaluation! Bring pencil #2 with eraser No use of calculator or any electronic device during the exam We provide the scantrons
Lines of Hydrogen. Most prominent lines in many astronomical objects: Balmer lines of hydrogen
The Family of Stars Lines of Hydrogen Most prominent lines in many astronomical objects: Balmer lines of hydrogen The Balmer Thermometer Balmer line strength is sensitive to temperature: Most hydrogen
Review III. ASTR 371, Fall Jovian Planets and Rings (Lecture Notes 9; Chap 12, 14)
ASTR 371, Fall 2016 Review III 9. Jovian Planets and Rings (Lecture Notes 9; Chap 12, 14) 9.1-2 Introduction, Motion a. Carefully study the data for the Jovian planets. Must know the general properties
Mar 22, INSTRUCTIONS: First ll in your name and social security number (both by printing
ASTRONOMY 0089: EXAM 2 Class Meets M,W,F, 1:00 PM Mar 22, 1996 INSTRUCTIONS: First ll in your name and social security number (both by printing and by darkening the correct circles). Sign your answer sheet
ASTR-1020: Astronomy II Course Lecture Notes Section III
ASTR-1020: Astronomy II Course Lecture Notes Section III Dr. Donald G. Luttermoser East Tennessee State University Edition 4.0 Abstract These class notes are designed for use of the instructor and students
1. Basic Properties of Stars
1. Basic Properties of Stars This is the Sun during a total eclipse. The Sun, our closest star, is very much representative of the objects that we will study during this module, namely stars. Much of the
Lecture 1: Introduction. Literature: Onno Pols chapter 1, Prialnik chapter 1
Lecture 1: Introduction Literature: Onno Pols chapter 1, Prialnik chapter 1!" Goals of the Course! Understand the global characteristics of stars! Relate relevant microphysics to the global stellar characteristics!
Book page cgrahamphysics.com Stellar Spectra
Book page 650-652 Stellar Spectra Emission and absorption Spectra The black lines of the absorption spectrum match up with the bright lines of the emission spectrum Spectra unique to each element Emission
Astr 5465 Feb. 6, 2018 Today s Topics
Astr 5465 Feb. 6, 2018 Today s Topics Stars: Binary Stars Determination of Stellar Properties via Binary Stars Classification of Binary Stars Visual Binaries Both stars visible Only one star visible Spectroscopic
Introduction The Role of Astronomy p. 3 Astronomical Objects of Research p. 4 The Scale of the Universe p. 7 Spherical Astronomy Spherical
Introduction The Role of Astronomy p. 3 Astronomical Objects of Research p. 4 The Scale of the Universe p. 7 Spherical Astronomy Spherical Trigonometry p. 9 The Earth p. 12 The Celestial Sphere p. 14 The
GALAXIES AND STARS. 2. Which star has a higher luminosity and a lower temperature than the Sun? A Rigel B Barnard s Star C Alpha Centauri D Aldebaran
GALAXIES AND STARS 1. Compared with our Sun, the star Betelgeuse is A smaller, hotter, and less luminous B smaller, cooler, and more luminous C larger, hotter, and less luminous D larger, cooler, and more
Pr P ope p rti t es s of o f St S a t rs
Properties of Stars Distances Parallax ( Triangulation ): - observe object from two separate points - use orbit of the Earth (1 AU) - measure angular shift of object - angle depends on distance to object
Observed Properties of Stars - 2 ASTR 2110 Sarazin
Observed Properties of Stars - 2 ASTR 2110 Sarazin Properties Location Distance Speed Radial velocity Proper motion Luminosity, Flux Magnitudes Magnitudes Stellar Colors Stellar Colors Stellar Colors Stars
MASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department. Quiz 2
MASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Physics 8.282 April 16, 2003 Quiz 2 Name SOLUTIONS (please print) Last First 1. Work any 7 of the 10 problems - indicate clearly which 7 you want
CHAPTER 29: STARS BELL RINGER:
CHAPTER 29: STARS BELL RINGER: Where does the energy of the Sun come from? Compare the size of the Sun to the size of Earth. 1 CHAPTER 29.1: THE SUN What are the properties of the Sun? What are the layers
The Distance Modulus. Absolute Magnitude. Chapter 9. Family of the Stars
Foundations of Astronomy 13e Seeds Phys1403 Introductory Astronomy Instructor: Dr. Goderya Chapter 9 Family of the Stars Cengage Learning 016 Topics for Today s Class 1. Recap: Intrinsic Brightness a)
Foundations of Astrophysics
Foundations of Astrophysics Barbara Ryden The Ohio State University Bradley M. Peterson The Ohio State University Preface xi 1 Early Astronomy 1 1.1 The Celestial Sphere 1 1.2 Coordinate Systems on a Sphere
Final Exam. Sample Questions. Final Exam. Which of the following statement is true? THE FINAL IS DECEMBER 15 th : 7-10pm!
THE FINAL IS DECEMBER 15 th : 7-10pm! Review Session Final Exam Date: Monday, Dec 15 th Place and Time: In the Greg 100 classroom 7pm until 10pm. The test is designed for 2 hours. Format: 80 multiple choice
StarTalk. Sanjay Yengul May "To know ourselves, we must know the stars."
StarTalk Sanjay Yengul May 2016 "To know ourselves, we must know the stars." Twinkle Twinkle How many stars are there? How big are these stars? Picture of night sky What are they made of? Why do they shine?
! p. 1. Observations. 1.1 Parameters
1 Observations 11 Parameters - Distance d : measured by triangulation (parallax method), or the amount that the star has dimmed (if it s the same type of star as the Sun ) - Brightness or flux f : energy
Chapter 15 Lecture. The Cosmic Perspective Seventh Edition. Surveying the Stars Pearson Education, Inc.
Chapter 15 Lecture The Cosmic Perspective Seventh Edition Surveying the Stars 15.1 Properties of Stars Our goals for learning: How do we measure stellar luminosities? How do we measure stellar temperatures?
Lecture 26 The Hertzsprung- Russell Diagram January 13b, 2014
1 Lecture 26 The Hertzsprung- Russell Diagram January 13b, 2014 2 Hertzsprung-Russell Diagram Hertzsprung and Russell found a correlation between luminosity and spectral type (temperature) 10000 Hot, bright
Lecture 21. Stellar Size
Lecture 21 Stellar Mass; The Main Sequence Visual and Spectroscopic Binaries Mass and the Main Sequence Explaining the Main Sequence Mar 8, 2006 Astro 100 Lecture 21 1 Stellar Size Taking ratios to the
18. Which graph best represents the relationship between the number of sunspots and the amount of magnetic activity in the Sun?
1. Which star has a surface temperature most similar to the surface temperature of Alpha Centauri? A) Polaris B) Betelgeuse C) Procyon B D) Sirius 2. Giant stars have greater luminosity than our sun mainly
MSci Astrophysics 210PHY412
MSci Astrophysics 210PHY412 Stellar structure and evolution Dr. Stephen Smartt (Room S039) Department of Physics and Astronomy S.Smartt@qub.ac.uk Online resources - QoL and http://star.pst.qub.ac.uk/~sjs/teaching.html
Astronomy December, 2016 Introduction to Astronomy: The Solar System. Final exam. Practice questions for Unit V. Name (written legibly):
Astronomy 101 12 December, 2016 Introduction to Astronomy: The Solar System Final exam Practice questions for Unit V Name (written legibly): Honor Pledge: On my honor, I have neither given nor received
Spectral Classification of Stars
Department of Physics and Geology Spectral Classification of Stars Astronomy 1402 Part 1: Background Spectral Classification of Stars 1.1 Spectral Types: O, B, A, F, G, K, M On a dark, clear night far
Characterizing Stars
Characterizing Stars 1 Guiding Questions 1. How far away are the stars? 2. What evidence do astronomers have that the Sun is a typical star? 3. What is meant by a first-magnitude or second magnitude star?
Characterizing Stars. Guiding Questions. Parallax. Careful measurements of the parallaxes of stars reveal their distances
Guiding Questions Characterizing Stars 1. How far away are the stars? 2. What evidence do astronomers have that the Sun is a typical star? 3. What is meant by a first-magnitude or second magnitude star?
Guiding Questions. Measuring Stars
Measuring Stars Guiding Questions 1. How far away are the stars? 2. What is meant by a first-magnitude or second magnitude star? 3. Why are some stars red and others blue? 4. What are the stars made of?
Reading and Announcements. Read Chapters 8.3, 11.5, 12.1 Quiz #5, Thursday, March 21 Homework #5 due Tuesday, March 19
Reading and Announcements Read Chapters 8.3, 11.5, 12.1 Quiz #5, Thursday, March 21 Homework #5 due Tuesday, March 19 Measurements of Star Properties Apparent brightness Direct measurement Parallax Distance
Properties of Stars. For such huge objects, stars have comparatively simple properties when seen from a long way off
Properties of Stars For such huge objects, stars have comparatively simple properties when seen from a long way off apparent magnitude distance and direction in space luminosity - absolute magnitude temperature
THIRD-YEAR ASTROPHYSICS
THIRD-YEAR ASTROPHYSICS Problem Set: Stellar Structure and Evolution (Dr Ph Podsiadlowski, Michaelmas Term 2006) 1 Measuring Stellar Parameters Sirius is a visual binary with a period of 4994 yr Its measured
Astronomy 102: Stars and Galaxies Examination 3 April 11, 2003
Name: Seat Number: Astronomy 102: Stars and Galaxies Examination 3 April 11, 2003 Do not open the test until instructed to begin. Instructions: Write your answers in the space provided. If you need additional
OTHER MOTIONS. Just so far away they appear to move very slowly
OTHER MOTIONS The position of a nearby star changing over a year gives us parallax Stars can also move on their own Real motion, not just our point of view They are just balls of gas and are moving around
Lecture 16 The Measuring the Stars 3/26/2018
Lecture 16 The Measuring the Stars 3/26/2018 Test 2 Results D C B A Questions that I thought were unfair: 13, 18, 25, 76, 77, 80 Curved from 85 to 79 Measuring stars How far away are they? How bright are
Measuring Radial & Tangential Velocity. Radial velocity measurement. Tangential velocity measurement. Measure the star s Doppler shift
17. The Nature of the Stars Parallax reveals stellar distance Stellar distance reveals luminosity Luminosity reveals total energy production The stellar magnitude scale Surface temperature determines stellar
Assignments for Monday Oct. 22. Read Ch Do Online Exercise 10 ("H-R Diagram" tutorial)
Assignments for Monday Oct. 22 Read Ch. 13 + Do Online Exercise 10 ("H-R Diagram" tutorial) Luminosity passing through each sphere is the same. Area of sphere: 4π(radius) 2 Divide luminosity by area to
Measuring the Properties of Stars (ch. 17) [Material in smaller font on this page will not be present on the exam]
![Measuring the Properties of Stars (ch. 17) [Material in smaller font on this page will not be present on the exam]](/thumbs/85/91935248.jpg "Measuring the Properties of Stars (ch. 17) [Material in smaller font on this page will not be present on the exam]")
Measuring the Properties of Stars (ch. 17) [Material in smaller font on this page will not be present on the exam] Although we can be certain that other stars are as complex as the Sun, we will try to
Astronomy Exam 3 - Sun and Stars
Astronomy Exam 3 - Sun and Stars Study online at quizlet.com/_4zgp6 1. `what are the smallest group of stars in the H-R diagram 2. A star has a parallax of 0.05". what is the distance from the earth? white
Stellar Astronomy Sample Questions for Exam 3
Stellar Astronomy Sample Questions for Exam 3 Chapter 7 1. A protostar is formed by a) the rapid expansion of gas from an exploding star. b) the gravitational collapse of a rotating interstellar cloud.
Chapter 15 Surveying the Stars. Properties of Stars. Parallax and Distance. Distances Luminosities Temperatures Radii Masses
hapter 15 Surveying the Stars Properties of Stars istances Luminosities s Radii Masses istance Use radar in Solar System, but stars are so far we use parallax: apparent shift of a nearby object against
Examination paper for FY2450 Astrophysics
1 Department of Physics Examination paper for FY2450 Astrophysics Academic contact during examination: Robert Hibbins Phone: 94 82 08 34 Examination date: 04-06-2013 Examination time: 09:00 13:00 Permitted
Astronomy 100 Spring 2006 Lecture Questions Twelve Weeks Review
Astronomy 100 Spring 2006 Lecture Questions Twelve Weeks Review 16-1 Fusion in the Sun The solar corona has temperatures roughly the same as temperatures in the Sun's core, where nuclear fusion takes place.
Science Olympiad Astronomy C Division Event National Exam
Science Olympiad Astronomy C Division Event National Exam University of Nebraska-Lincoln May 15-16, 2015 Team Number: Team Name: Instructions: 1) Please turn in all materials at the end of the event. 2)
Measuring the Stars. The measurement of distances The family of distance-measurement techniques used by astronomers to chart the universe is called
Measuring the Stars How to measure: Distance Stellar motion Luminosity Temperature Size Evolutionary stage (H-R diagram) Cosmic distances Mass The measurement of distances The family of distance-measurement
Lecture Outlines. Chapter 17. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.
Lecture Outlines Chapter 17 Astronomy Today 8th Edition Chaisson/McMillan Chapter 17 Measuring the Stars Units of Chapter 17 17.1 The Solar Neighborhood 17.2 Luminosity and Apparent Brightness 17.3 Stellar
Astronomy 1 Fall 2016
Astronomy 1 Fall 2016 Announcement: Tonight s observing session with Stephanie Ho has been CANCELLED. She has rescheduled it for 8-9pm on Thursday Nov. 3 rd. Hopefully the clouds will part by then. Lecture
Observed Properties of Stars - 2 ASTR 2120 Sarazin
Observed Properties of Stars - 2 ASTR 2120 Sarazin Properties Location Distance Speed Radial velocity Proper motion Luminosity, Flux Magnitudes Magnitudes Hipparchus 1) Classified stars by brightness,
Astronomy. The Nature of Stars
Astronomy A. Dayle Hancock adhancock@wm.edu Small 239 Office hours: MTWR 10-11am The Nature of Stars Distances to stars A Star's brightness and Luminosity A Magnitude scale Color indicates a Star's temperature
λ = 650 nm = c = m s 1 f =? c = fλ f = c λ = ( m s 1 ) ( m) = = Hz T = 1 f 4.
Chapter 13 Stars Section 13.1 Astronomical measurements Worked example: Try yourself 13.1.1 CALCULATING THE FREQUENCY AND PERIOD OF LIGHT The speed of light in a vacuum is approximately 3.0 10 8 m s 1.
Chapter 11 Surveying the Stars
Chapter 11 Surveying the Stars Luminosity Luminosity: Rate of energy emitted by star every second. Apparent brightness (flux): Amount of energy passing through every second per unit area. Luninosity =
Determining the Properties of the Stars
Determining the Properties of the Stars This set of notes by Nick Strobel covers: The properties of stars--their distances, luminosities, compositions, velocities, masses, radii, and how we determine those
Stars, Galaxies & the Universe Announcements. Stars, Galaxies & the Universe Observing Highlights. Stars, Galaxies & the Universe Lecture Outline
Stars, Galaxies & the Universe Announcements Lab Observing Trip Next week: Tues (9/28) & Thurs (9/30) let me know ASAP if you have an official conflict (class, work) - website: http://astro.physics.uiowa.edu/~clang/sgu_fall10/observing_trip.html
Stellar Models ASTR 2110 Sarazin
Stellar Models ASTR 2110 Sarazin Jansky Lecture Tuesday, October 24 7 pm Room 101, Nau Hall Bernie Fanaroff Observing the Universe From Africa Trip to Conference Away on conference in the Netherlands
Proton-proton cycle 3 steps PHYS 162 1
Proton-proton cycle 3 steps PHYS 162 1 4 Layers of the Sun CORE : center, where fusion occurs RADIATION: energy transfer by radiation CONVECTION: energy transfer by convection PHOTOSPHERE: what we see
days to rotate in its own axis km in diameter ( 109 diameter of the Earth ) and kg in mass ( mass of the Earth)
The Sun - It is located at the centre of our solar system with all planets and objects (comets and asteroids) revolving around it Page 1 of 6 - It s gravitational pull keeps the planets and other objects
Examination paper for FY2450 Astrophysics
1 Department of Physics Examination paper for FY2450 Astrophysics Academic contact during examination: Rob Hibbins Phone: 94820834 Examination date: 01-06-2015 Examination time: 09:00 13:00 Permitted examination
while the Planck mean opacity is defined by
PtII Astrophysics Lent, 2016 Physics of Astrophysics Example sheet 4 Radiation physics and feedback 1. Show that the recombination timescale for an ionised plasma of number density n is t rec 1/αn where
Binary Stars (continued) ASTR 2120 Sarazin. γ Caeli - Binary Star System
Binary Stars (continued) ASTR 2120 Sarazin γ Caeli - Binary Star System Visual Binaries: Types of Binary Stars Spectroscopic Binaries: Eclipsing Binaries: Periodic changes in brightness, stars block one
Parallax: Measuring the distance to Stars
Measuring the Stars Parallax: Measuring the distance to Stars Use Earth s orbit as baseline Parallactic angle = 1/2 angular shift Distance from the Sun required for a star to have a parallactic angle of
Each star is born with a specific mass. This mass is the main factor in determining the star s brightness, temperature, expected lifetime, type of
Each star is born with a specific mass. This mass is the main factor in determining the star s brightness, temperature, expected lifetime, type of death, and spectra. Stars are classified according to
ASTRONOMY CURRICULUM Unit 1: Introduction to Astronomy
Chariho Regional School District - Science Curriculum September, 2016 ASTRONOMY CURRICULUM Unit 1: Introduction to Astronomy OVERVIEW Summary Students will be introduced to the overarching concept of astronomy.
MASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Earth, Atmospheric, and Planetary Sciences Department. Problem Set 6
MASSACHUSETTS INSTITUTE OF TECHNOLOGY Physics Department Earth, Atmospheric, and Planetary Sciences Department Astronomy 8.282J 12.402J March 17, 2006 Problem Set 6 Due: Friday, March 24 (in lecture) Reading:
Review Chapter 10. 2) A parsec is slightly more than 200,000 AU. 2)
Review Chapter 10 TRUE/FALSE. Write 'T' if the statement is true and 'F' if the statement is false. 1) A parsec is about 3.3 light-years. 1) 2) A parsec is slightly more than 200,000 AU. 2) 3) The nearest
Organizing the Family of Stars:
Organizing the Family of Stars: We know: Stars have different temperatures, different luminosities, and different sizes. To bring some order into that zoo of different types of stars: organize them in
ASTR2050: Introductory Astronomy and Astrophysics Syllabus for Spring 1999 January 4, 1999
ASTR2050: Introductory Astronomy and Astrophysics Syllabus for Spring 1999 January 4, 1999 This is a working document and will change periodically. It outlines the topics that will be covered during the
Astronomy 210 Spring 2017: Quiz 5 Question Packet 1. can: 2. An electron moving between energy levels
Permitted energy levels Astronomy 210 Spring 2017: Quiz 5 Question Packet 1 1. An electron in energy level 1 2 can: (A) only emit a photon. (B) only absorb a photon. (C) either emit, or absorb a photon.
Stellar Spectrum Classification Lab Activity
Stellar Spectrum Classification Lab Activity Directions In this exercise you will be given a table of the standard spectral classes and a number of sample spectra to be used as the accepted spectra. While
Chapter 15 Surveying the Stars Pearson Education, Inc.
Chapter 15 Surveying the Stars 15.1 Properties of Stars Our goals for learning: How do we measure stellar luminosities? How do we measure stellar temperatures? How do we measure stellar masses? 1. How
Measuring Radial & Tangential Velocity. Radial velocity measurement. Tangential velocity measurement. Measure the star s Doppler shift
17. The Nature of the Stars Parallax reveals stellar distance Stellar distance reveals luminosity Luminosity reveals total energy production The stellar magnitude scale Surface temperature determines stellar
Return both exam and scantron sheet when you leave the gym
BROCK UNIVERSITY Page 1 of 17 Final Exam December 2017 Number of pages: 17 Course: ASTR 1P01, Section 1 Number of Students: 465 Date of Examination: December 13, 2017 Number of hours: 2 Time of Examination:
ASTR Look over Chapter 15. Good things to Know. Triangulation
ASTR 1020 Look over Chapter 15 Good things to Know Triangulation Parallax Parsecs Absolute Visual Magnitude Distance Modulus Luminosity Balmer Lines Spectral Classes Hertzsprung-Russell (HR) diagram Main
HW 5 posted. Deadline: * Monday 3.00 PM * -- Tip from the coach: Do it earlier, as practice for mid term (it covers only parts included in exam).
Admin HW 5 posted. Deadline: * Monday 3.00 PM * -- Tip from the coach: Do it earlier, as practice for mid term (it covers only parts included in exam). Lab Wednesday/Thursday -- Spectra http://jonsundqvist.com/phys133/labs.html
II Planet Finding.
II Planet Finding http://sgoodwin.staff.shef.ac.uk/phy229.html 1.0 Introduction There are a lot of slides in this lecture. Much of this should be familiar from PHY104 (Introduction to Astrophysics) and
USAAAO First Round 2015
USAAAO First Round 2015 This round consists of 30 multiple-choice problems to be completed in 75 minutes. You may only use a scientific calculator and a table of constants during the test. The top 50%