PHY2083 ASTRONOMY. Dr. Rubina Kotak Office F016. Dr. Chris Watson Office S036
|
|
- Stella Beasley
- 5 years ago
- Views:
Transcription
1 PHY2083 ASTRONOMY Dr. Rubina Kotak Office F016 Dr. Chris Watson Office S036
2 PHY2083 ASTRONOMY Weeks 1-6: Monday 10:00 DBB 0G.005 Wednesday 9:00 PFC 02/018 Friday 10:00 DBB 0G.005
3 Preliminaries: Module relies on use of previous maths, physics knowledge! Units: astronomy units e.g. distances in AU or pc not metres; solar masses, luminosities pdf files of lecture notes (summary) will be made available on QoL before the lectures in as far as possible. You should bring these to the lectures and annotate as required. The pdf files will NOT necessarily contain all the material discussed in the lectures => attend the lectures and supplement the notes with textbooks! Bring your calculator to the lectures! Feedback welcome! Have fun! Ask questions!
4 Assignments You will be given 2 assignments to complete over the course of the next 6 weeks. These will count for 10% of your module mark (also, good practice for exams!)
5 Plan for today Scales in the Universe Useful units (AU, light-year etc.) Basic concepts: parallax; radial velocities
6 Units of distance Why can t we simply use metres / kilometres / miles?
7 Astronomical Unit (AU) = mean Earth-Sun distance = m ~ 1.49 x m 1 AU AUs are useful for distances within the solar system e.g. Mercury ~ 0.39 AU; Neptune ~ 30 AU (from Sun)
8 A few basic concepts: Maxwell Einstein The speed of light is finite and constant ~ km/s
9 The speed of light is finite and constant But for everyday purposes, light appears to travel instantaneously 1m
10 Light-year (ly) Unit of distance, not time! 1 ly = distance travelled by light in 1 year: 1 year = d = 24 x 60 x 60 x s = s speed of light = 2.99 x 10 8 m/s (distance = speed x time) => 1 ly = 2.99 x 10 8 x = 9.43 x m ~ AU
11 It takes about 8 minutes for light from the Sun to reach us
12 Saturn: 1.4 billion km => 1.3 light-hours NASA
13 The speed of light is finite and constant => looking far out in space = looking back in time Light from Alpha Cen takes 4 years to reach us.
14 Virgo cluster of galaxies ~ 53 million light years away
15 The most distant object in the Universe is in this image! light from it has travelled 13.2 billion yrs
16 Examples of distances in ly: Nearest star to the solar system: Proxima Centauri ~ 4.2 ly Sirius: brightest star in the night sky ~ 8.6 ly Our galaxy (Milky Way) is about 1000 ly across The Andromeda galaxy (sister galaxy to Milky Way) ~ 2.5 x 10 6 ly Need a more manageable unit for distances to other galaxies
17 Parsec (pc) (see later for definition of parsec) 1 pc = AU ~ 3.26 ly Distances to galaxies, clusters of galaxies etc. given typically in kilo-parsecs (kpc) i.e., 10 3 pc, and mega-parsecs (Mpc) i.e., 10 6 pc
18 8200 pc Solar System
19 Velocities of celestial bodies Earth s Orbital Velocity v=29.8 km/sec
20 220 km/sec
21 A binary stellar system:
22 Angular measures I (used for distances, velocities) Size and scale are often specified by measuring lengths and angles. A full circle contains 360 degrees = 2π radians Each 1 degree increment can be sub-divided into arc minutes i.e., 60 arc minutes (60 ) = 1 degree Each arc minute can be divided into arc seconds i.e., 60 arc seconds (60 ) = 1 arc minute
23 Consider the velocity of a star relative to an observer V θ C v s B Vs can be decomposed into 2 mutually perpendicular components A v r D V r = AD = radial velocity; component along line-of-sight V θ = AC = transverse / tangential velocity; projected angular motion V s = AB = space velocity; motion of star relative to the sun
24 Proper Motion The angular distance a star appears to move in a year (after correction for the motion of the Earth) is its PROPER MOTION, µ. Measured in arc seconds per year. Most stars are too distant to have an appreciable µ. Largest value is for Barnard s star at 10.3 / yr
25 Barnard s star
26 Parallax Apparent change in direction of a star due to the orbital motion of the Earth around the Sun. On Earth, the distance to the peak of a distant mountain can be determined by measuring the angular position of the peak from 2 observation points separated by a known baseline distance. Distance to the peak follows from simple trigonometry. Triangulation
27 Triangulation d = B / (tan p) Of course, finding the distance to a star requires a baseline longer than the Earth s diameter. As the Earth orbits the sun, baseline = diameter of Earth s orbit around the Sun
28
29 Angular measures II (used for distances, velocities) 1 radian ~ 57.3 degrees ~ 3438 (arc mins) ~ (arc secs) 1 pc = AU ~ 3.26 ly A parsec is the distance at which the parallax of an object = 1 arcsecond distance (pc) = 1 / parallax (arcsecs)
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
More information5. A particular star has an angle of parallax of 0.2 arcsecond. What is the distance to this star? A) 50 pc B) 2 pc C) 5 pc D) 0.
Name: Date: 1. How far away is the nearest star beyond the Sun, in parsecs? A) between 1 and 2 pc B) about 12 pc C) about 4 pc D) between 1/2 and 1 pc 2. Parallax of a nearby star is used to estimate its
More informationBasic Properties of the Stars
Basic Properties of the Stars The Sun-centered model of the solar system laid out by Copernicus in De Revolutionibus (1543) made a very specific prediction: that the nearby stars should exhibit parallax
More informationStellar distances and velocities. ASTR320 Wednesday January 24, 2018
Stellar distances and velocities ASTR320 Wednesday January 24, 2018 Special public talk this week: Mike Brown, Pluto Killer Wednesday at 7:30pm in MPHY204 Why are stellar distances important? Distances
More informationDistance and Size of a Celestial Body
PHYS 320 Lecture 2 Distance and Size of a Celestial Body Jiong Qiu MSU Physics Department Wenda Cao NJIT Physics Department Outline q Lecture 2 Distance and Size of a Celestial Body n n n n n n n n 2.1
More informationAstronomy 111. Dr. Joseph E. Pesce, Ph.D. Introduction. Introduction 8/28/14. Astronomy & Astrophysics. Our understanding is based on laws of physics:
8/28/14 Astronomy 111 Dr. Joseph E. Pesce, Ph.D. 1-4 Introduction Astronomy & Astrophysics Introduction ASTRON = Star NOMOS = Law PHYSIC = Nature 1-5 ³ Astronomy: observable properties of objects in the
More informationPARALLAX AND PROPER MOTION
PARALLAX AND PROPER MOTION What will you learn in this Lab? We will be introducing you to the idea of parallax and how it can be used to measure the distance to objects not only here on Earth but also
More informationAST 301: Topics for today!
AST 301: Topics for today! 1.! Syllabus. You should have read the syllabus in detail. So only brief questions about course, grading, etc. today.!!!go to the course web site and bookmark it as soon as possible.!
More informationHow to Understand Stars Chapter 17 How do stars differ? Is the Sun typical? Location in space. Gaia. How parallax relates to distance
How to Understand Stars Chapter 7 How do stars differ? Is the Sun typical? Image of Orion illustrates: The huge number of stars Colors Interstellar gas Location in space Two dimensions are easy measure
More informationIntroduction To Modern Astronomy I: Solar System
ASTR 111 003 Fall 2007 Lecture 01 Aug. 27, 2007 Introduction To Modern Astronomy I: Solar System Introducing Astronomy (chap. 1-6) Planets and Moons (chap. 7-15) Chap. 16: Our Sun Chap. 28: Search for
More informationCharacterizing Stars
Characterizing Stars The stars Every star you see in the sky is a large hot ball of gas like our star the Sun. Each one possibly making up a solar system with planets and debris orbiting around them. Stellar
More informationStructure & Evolution of Stars 1
Structure and Evolution of Stars Lecture 2: Observational Properties Distance measurement Space velocities Apparent magnitudes and colours Absolute magnitudes and luminosities Blackbodies and temperatures
More informationThe Scale of the Cosmos
The Scale of the Cosmos Scale defined as relative magnitude. Astronomy deals with objects on a vast range of size scales and time scales. Most of these size and time scales are way beyond our every-day
More informationThe Scale of the Cosmos
The Scale of the Cosmos Scale defined as relative magnitude. Astronomy deals with objects on a vast range of size scales and time scales. Most of these size and time scales are way beyond our every-day
More informationPhys 214. Planets and Life
Phys 214. Planets and Life Dr. Cristina Buzea Department of Physics Room 259 E-mail: cristi@physics.queensu.ca (Please use PHYS214 in e-mail subject) Lecture 6. The Structure and Scale of the Universe
More informationAST 301: What you will have to learn and get used to 1. Basic types of objects in the universe
AST 301: What you will have to learn and get used to 1. Basic types of objects in the universe Planets, stars, galaxies, a few things inbetween--look through your textbook soon! You will have to learn:
More informationThe Stars. Background & History The Celestial Sphere: Fixed Stars and the Luminaries
The Stars Background & History The Celestial Sphere: Fixed Stars and the Luminaries The Appearance of Stars on the Sky Brightness and Brightness Variations Atmospheric Effects: Twinkling Variable Stars
More informationAstronomy 150: Killer Skies. Lecture 20, March 7
Assignments: Astronomy 150: Killer Skies HW6 due next time at start of class Lecture 20, March 7 Office Hours begin after class or by appointment Night Observing continues this week, 7-9 pm last week!
More informationAstronomy 114. Lecture 2: Measurement, astronomical distance. Martin D. Weinberg. UMass/Astronomy Department
Astronomy 114 Lecture 2: Measurement, astronomical distance Martin D. Weinberg weinberg@astro.umass.edu UMass/Astronomy Department A114: Lecture 2 31 Jan 2007 Read: Ch. 1-2 Astronomy 114 1/18 Announcements
More informationHow big is the Universe and where are we in it?
Announcements Results of clicker questions from Monday are on ICON. First homework is graded on ICON. Next homework due one minute before midnight on Tuesday, September 6. Labs start this week. All lab
More informationASTR 1010 Astronomy of the Solar System. Course Info. Course Info. Fall 2006 Mon/Wed/Fri 11:00-11:50AM 430 Aderhold Learning Center
ASTR 1010 Astronomy of the Solar System Fall 2006 Mon/Wed/Fri 11:00-11:50AM 430 Aderhold Learning Center Instructor: Wes Ryle Course Info In-class Activities/Quizzes (10%) 4 Homework Assignments (15%)
More informationPhys 214. Planets and Life
Phys 214. Planets and Life Dr. Cristina Buzea Department of Physics Room 259 E-mail: cristi@physics.queensu.ca (Please use PHYS214 in e-mail subject) Lecture 13. Midterm review February 4th, 2008 1. Astronomy
More informationDistances to Stars. Important as determines actual brightness but hard to measure as stars are so far away
SECTION II: Nature of Stars Astronomers measure properties of Stars Distance Mass Apparent Brightness Surface Temperature Radius Find that some are related Large Mass Large Absolute Brightness We will
More informationChapter 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 =
More informationINTRODUCTION TO STARS,
ASTR& 115: STARS, GALAXIES, AND THE COSMOS This work is a derivative of the Astronomy textbook by OpenStax, licensed under CC BY 4.0. Except where otherwise noted, this work is licensed under CC BY 4.0
More informationLecture 1. ASTR 111 Section 002 Introductory Astronomy Solar System. Dr. Weigel. Outline. Course Overview Topics. Course Overview General Information
Lecture 1 Course Overview Topics ASTR 111 Section 002 Introductory Astronomy Solar System Dr. Weigel Outline 1.1 Course Overview 1.2 Course Logistics and Syllabus 1.3 Angular Measurements 1.4 Accuracy
More informationThe Flammarion engraving by an unknown artist, first documented in Camille Flammarion's 1888 book L'atmosphère: météorologie populaire.
The Flammarion engraving by an unknown artist, first documented in Camille Flammarion's 1888 book L'atmosphère: météorologie populaire. Horizon Coordinates: Altitude (angular height above horizon) Azimuth
More informationChapter 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
More informationObserved Properties of Stars ASTR 2120 Sarazin
Observed Properties of Stars ASTR 2120 Sarazin Extrinsic Properties Location Motion kinematics Extrinsic Properties Location Use spherical coordinate system centered on Solar System Two angles (θ,φ) Right
More informationAstronomy 102: Stars and Galaxies Review Exam 3
October 31, 2004 Name: Astronomy 102: Stars and Galaxies Review Exam 3 Instructions: Write your answers in the space provided; indicate clearly if you continue on the back of a page. No books, notes, or
More informationThe Cosmological Distance Ladder. It's not perfect, but it works!
The Cosmological Distance Ladder It's not perfect, but it works! First, we must know how big the Earth is. Next, we must determine the scale of the solar system. Copernicus (1543) correctly determined
More informationAstronomy, Astrophysics, and Cosmology
Astronomy, Astrophysics, and Cosmology Luis A. Anchordoqui Department of Physics and Astronomy Lehman College, City University of New York Lesson I February 2, 2016 arxiv:0706.1988 L. A. Anchordoqui (CUNY)
More informationHOMEWORK - 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
More informationAstronomy 102: Stars and Galaxies Sample Review Test for Examination 3
October 28, 2003 Name: Astronomy 102: Stars and Galaxies Sample Review Test for Examination 3 Do not open the test until instructed to begin. Instructions: Write your answers in the space provided. No
More informationAstronomy 9 Concepts of the Cosmos
Astronomy 9 Concepts of the Cosmos Monday/Wednesday, 1:30-2:45 pm, Cabot Auditorium LECTURE 2: I.Our Place in the Universe Lecture on Mon., Feb. 1 st Pre-course Test - REQUIRED! (if you want the attendance
More informationMeasuring Distances. Taking the Measure of the Universe
Measuring Distances Taking the Measure of the Universe The Importance of Distance We talked about how the brightness of a star can be due to 2 effects: distance or luminosity. Without a direct measurement
More informationPH104 Lab 2 Measuring Distances Pre-Lab
Name: Lab Time: PH04 Lab 2 Measuring Distances Pre-Lab 2. Goals This is the second lab. Like the first lab this lab does not seem to be part of a complete sequence of the study of astronomy, but it will
More informationThe Universe April 2, Lecture 2 1
Beyond Our Comfort Zone Direct Experience: 10-5 to 10 5 meters Dust grain may have 0.01 mm = 10 micron diameter View from mountaintop may extend 100 km Experts may claim comfort with 10-7 to 10 7 m Optical
More informationTHE SIZE AND SCALE OF THE UNIVERSE
1 THE SIZE AND SCALE OF THE UNIVERSE 1. Scientific notation review Write the following in proper scientific notation, giving the proper number of significant figures. 1.a Thirty-one million, seven hundred
More informationStars I. Distance and Magnitude. How Does One Measure Distance? Distances. Stellar Parallax. Distance Equation some examples!
Stars I Distance and Magnitude Chapter 17 Why doesn t comparison work? Distances The nearest star (Alpha Centauri) is 40 trillion kilometers away(4 ly) Distance is one of the most important quantities
More informationA Sense of Scale and The Motions of Earth. The guitar player Pablo Picasso (1910)
A Sense of Scale and The Motions of Earth The guitar player Pablo Picasso (1910) Announcements n Notes from the first lecture are available on the class web site (www.astro.umass.edu/~calzetti/astro100).
More informationTAKEN FROM HORIZONS 7TH EDITION CHAPTER 1 TUTORIAL QUIZ
TAKEN FROM HORIZONS 7TH EDITION CHAPTER 1 TUTORIAL QUIZ 1. If the solar system is scaled down so that the Sun is represented by a basketball, a. a ping-pong ball located 500 feet away would properly represent
More informationASTRONOMY 202 Spring 2007: Solar System Exploration
ASTRONOMY 202 Spring 2007: Solar System Exploration Instructor: Dr. David Alexander Web-site: www.ruf.rice.edu/~dalex/astr202_s07 Class 3: Our Place in the Universe [1/19/07] Announcements Scale in the
More informationOPTION 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
More informationAST 301, Lecture 1. James Lattimer. Department of Physics & Astronomy 449 ESS Bldg. Stony Brook University. January 23, 2017
AST 301, Lecture 1 James Lattimer Department of Physics & Astronomy 449 ESS Bldg. Stony Brook University January 23, 2017 Cosmic Catastrophes (AKA Collisions) james.lattimer@stonybrook.edu Course Components
More informationLecture 3: Chapter 1- Charting the Heavens. Assignment: Read Chapter 1 of Astronomy Today
Lecture 3: Chapter 1- Charting the Heavens Assignment: Read Chapter 1 of Astronomy Today 1.2 Scientific Theory and the Scientific Method Scientific number notation Measures of Distance 1.2 Scientific
More informationThe Sun: Source of Heat & Light
Swinburne Online Education Exploring the Solar System Module 19: The Sun Activity 1: The Sun: Source of Heat & Light Swinburne University of Technology Summary: In this Activity, we will investigate (a)
More informationAy 1 Lecture 2. Starting the Exploration
Ay 1 Lecture 2 Starting the Exploration 2.1 Distances and Scales Some Commonly Used Units Distance: Astronomical unit: the distance from the Earth to the Sun, 1 au = 1.496 10 13 cm ~ 1.5 10 13 cm Light
More informationAstronomy 1010: Survey of Astronomy. University of Toledo Department of Physics and Astronomy
Astronomy 1010: Survey of Astronomy University of Toledo Department of Physics and Astronomy Information Kathy Shan Office: MH 4008 Phone: 530 2226 Email: kathy.shan@utoledo.edu Email is the best way to
More informationLecture 12: Distances to stars. Astronomy 111
Lecture 12: Distances to stars Astronomy 111 Why are distances important? Distances are necessary for estimating: Total energy released by an object (Luminosity) Masses of objects from orbital motions
More informationCOSMOLOGY 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
More informationOPTION 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
More informationPHY 475/375. Lecture 2. (March 28, 2012) The Scale of the Universe: The Shapley-Curtis Debate
PHY 475/375 Lecture 2 (March 28, 2012) The Scale of the Universe: The Shapley-Curtis Debate By the 1920 s a debate had developed over whether some of the spiral nebulae catalogued in the 18th century by
More informationPage # Astronomical Distances. Lecture 2. Astronomical Distances. Cosmic Distance Ladder. Distance Methods. Size of Earth
Size of Astronomical istances ecture 2 Astronomical istances istance to the Moon (1 sec) istance to the Sun (8 min) istance to other stars (years) istance to centre of our Galaxy ( 30,000 yr to centre)
More informationParallax: 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
More informationWelcome Astronomy Students Mr. Goodyear
Welcome Astronomy Students Mr. Goodyear Today s Objectives: S.W.B.A.T. Help teacher fill in seating chart with student picture/name and class attendance. Review classroom routines and expectations Complete
More informationLecture 29. Our Galaxy: "Milky Way"
Lecture 29 The Milky Way Galaxy Disk, Bulge, Halo Rotation Curve Galactic Center Apr 3, 2006 Astro 100 Lecture 29 1 Our Galaxy: "Milky Way" Milky, diffuse band of light around sky known to ancients. Galileo
More informationAstronomy 1143 Homework 1
Astronomy 43 Homework October 7, 205. Two Martian astronomers, Marvin and Marla, are located due north and south of each other on the planet Mars. Marvin sees the Sun directly overhead (at the zenith)
More informationAstronomical Measurements: Brightness-Luminosity-Distance-Radius- Temperature-Mass. Dr. Ugur GUVEN
Astronomical Measurements: Brightness-Luminosity-Distance-Radius- Temperature-Mass Dr. Ugur GUVEN Space Science Distance Definitions One Astronomical Unit (AU), is the distance from the Sun to the Earth.
More informationAST 301 Cosmic Collisions (AKA Collisions)
AST 301 Cosmic Collisions (AKA Collisions) James Lattimer lattimer@astro.sunysb.edu Department of Physics & Astronomy 461 ESS Bldg. Stony Brook University Lattimer, AST 301, Lecture 1 p.1/11 Course Components
More informationKEELE UNIVERSITY SCHOOL OF CHEMICAL AND PHYSICAL SCIENCES Year 1 ASTROPHYSICS LAB. WEEK 1. Introduction
KEELE UNIVERSITY SCHOOL OF CHEMICAL AND PHYSICAL SCIENCES Year 1 ASTROPHYSICS LAB WEEK 1. Introduction D. E. McLaughlin January 2011 The purpose of this lab is to introduce you to some astronomical terms
More information10/20/2009. Giants, Dwarfs, and the Main Sequences. My Office Hours: Tuesday 3:30 PM - 4:30 PM 206 Keen Building. The Sun and the Stars
the The Sun and the Giants, Dwarfs, and the Main Sequences 10/20/2009 My Office Hours: Tuesday 3:30 PM - 4:30 PM 206 Keen Building the Outline 1 2 3 the Outline 1 2 3 the Solar Structure Interior structure
More informationASTR-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
More informationPhysics Lab #10:! Stellar Parallax!
opposite Physics 10293 Lab #10: Stellar Parallax Introduction Parallax is a distance determination technique that uses geometry to measure the distance to some object when other means (such as a ruler
More informationObservational Astronomy - Lecture 13 Evolution of the Universe and Final Review
Observational Astronomy - Lecture 13 Evolution of the Universe and Final Review Craig Lage New York University - Department of Physics craig.lage@nyu.edu May 12, 2014 1 / 22 Remaining course logistics
More informationMeasuring Distances in Space
Measuring Distances in Space Textbook pages 396 405 Section 11.3 Summary Before You Read Looking at stars is like looking into the past. What might be the reason why? Record your thoughts on the lines
More informationProperties of Stars (continued) Some Properties of Stars. What is brightness?
Properties of Stars (continued) Some Properties of Stars Luminosity Temperature of the star s surface Mass Physical size 2 Chemical makeup 3 What is brightness? Apparent brightness is the energy flux (watts/m
More informationGet ready for quiz # 5! Get out a ½ sheet and Calculator
Get ready for quiz # 5! Get out a ½ sheet and Calculator The above image shows the solar eclipse earlier this month as covered and uncovered by several different solar observatories. The innermost image
More informationObservational Astronomy Astro-25. Professor Meyer-Canales Saddleback College
Observational Astronomy Astro-25 Professor Meyer-Canales Saddleback College Astronomy Courses Offered at Saddleback College Astronomy 20 - General Astronomy Survey/Lecture course Astronomy 21 - Solar System
More informationSpace Cruise & Picture Book
Space Cruise & Picture Book Learning Target: Recognize that there are enormous distances between objects in space Apply our knowledge of light and space travel to understand this distance. Watch Powers
More informationAstronomy 122 Outline
Astronomy 122 Outline This Class (Lecture 12): Stars Next Class: The Nature of Stars Homework #5 is posted. Nightlabs have started! Stellar properties Parallax (distance) Colors Spectral Classes Music:
More informationIntroductory Astronomy
1 Introductory Astronomy NAME: Homework 19: Some Star Basics: Homeworks and solutions are posted on the course web site. Homeworks are NOT handed in and NOT marked. But many homework problems ( 50 70 %)
More informationProf. Jeff Kenney Class 1 May 28, 2018
www.astro.yale.edu/astro120 Prof. Jeff Kenney Class 1 May 28, 2018 Lec 1-5: Lec 6-8: Astronomy 120 intro, physics review stars Lec 9-14: galaxies, clusters & dark matter Lec 15-18: active galaxies & black
More informationASTRONOMY 2 Overview of the Universe Second Practice Problem Set Solutions
ASTRONOMY 2 Overview of the Universe Second Practice Problem Set Solutions 1. Consider a 2 M neutron star. The mass of a neutron is 1.67 10 24 g, and 1 M = 2 10 33 g. (i) How many neutrons are in this
More informationLight and Stars ASTR 2110 Sarazin
Light and Stars ASTR 2110 Sarazin Doppler Effect Frequency and wavelength of light changes if source or observer move Doppler Effect v r dr radial velocity dt > 0 moving apart < 0 moving toward Doppler
More informationAngles and Units in Astronomy
Angles and Units in Astronomy Announcements Homework is due next Thursday (8/31/2017) 9 th and 10 th edition have the same question numbers Read Chapter 2 before next Tuesday My office hours are on Mondays
More informationAST 103 The Solar System
AST 103 The Solar System Prof. Ken Nagamine Dept. of Physics & Astronomy UNLV Pick up two items from the front table (one each): 1. Syllabus 2. ABCD card 1 Instructor Contact Info Prof. Ken Nagamine Office:
More informationTest #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
More informationPHYS 101: Elementary Astronomy. Dr. Jared Workman
PHYS 101: Elementary Astronomy Dr. Jared Workman Introductions - I ll go first Who are you Introduce yourself to 2 neighbors: Trade names, hometowns, interests, etc. Why are you taking this course? What
More informationLight. Geometric Optics. Parallax. PHY light - J. Hedberg
Light 1. Geometric Optics 1. Parallax 2. Magnitude Scale 1. Apparent Magnitude 2. Describing Brightness 3. Absolute Magnitude 3. Light as a Wave 1. Double Slit 2. The Poynting Vector 4. Blackbody Radiation
More informationHubble s Law and the Cosmic Distance Scale
Lab 7 Hubble s Law and the Cosmic Distance Scale 7.1 Overview Exercise seven is our first extragalactic exercise, highlighting the immense scale of the Universe. It addresses the challenge of determining
More informationDeAnza College Winter First Midterm Exam MAKE ALL MARKS DARK AND COMPLETE.
FAMILY NAME : (Please PRINT!) GIVEN NAME : (Please PRINT!) Signature: ASTRONOMY 4 DeAnza College Winter 2018 First Midterm Exam MAKE ALL MARKS DARK AND COMPLETE. Instructions: 1. On your Parscore sheet
More informationAstronomical Distance Determination
Distance ladder: Determine distances, d 1, for a nearby set of objects using technique 1, but then Astronomical Distance Determination http://apod.nasa.gov/apod/ Find new brighter objects at distances
More informationLab Title: Parallax and Astronomical Distances. Equipment: Sextant Meter sticks (or tape measures) Calipers Magnetic compasses.
Lab Title: Parallax and Astronomical Distances Equipment: Sextant Meter sticks (or tape measures) Calipers Magnetic compasses Introduction: Since we cannot travel to most celestial objects in order to
More informationAstronomy 122 TR Chemistry Annex. Outline. Power of Tens: Adding another Zero
Leslie Looney Phone: 244-3615 Email: lwlw@wuiucw. wedu Office: Astro Building #218 Office Hours: W 11:00 a.m noon or by appointment Astronomy 122 TR 1300-1350 112 Chemistry Annex This Class (Lecture 2):
More informationExplain why miles cannot be used to measure distances in space.
Space SC.8.E.5.1 SC.8.E.5.1: Recognize that there are enormous distances between objects in space and apply our knowledge of light and space travel to understand this difference. Essential Questions: Distances
More informationAstronomy 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
More informationAstro 13 Galaxies & Cosmology LECTURE 4 Tues 18 Jan 2011 P. Madau. I Cosmological Principles 25m II Why is the Sky Dark? (Olber s
Astro 13 Galaxies & Cosmology LECTURE 4 Tues 18 Jan 2011 P. Madau 20m I Cosmological Principles 25m II Why is the Sky Dark? (Olber s Paradox) 10m III Break 15m IV Expanding Univ. - Hubble Constant 20m
More informationMeasuring 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
More informationClassAction: Stellar Properties Module Instructor s Manual
ClassAction: Stellar Properties Module Instructor s Manual Table of Contents Section 1: Warm-up Questions...3 Temperature and Color.....4 Section 2: General Questions.....5 Apparent Magnitude and Brightness....6
More informationAstronomical Distance Determination.
Astronomical Distance Determination http://apod.nasa.gov/apod/ Distance ladder (beyond the AU): Determine distances, d 1, for some nearby set of objects using technique 1, but then Find new brighter objects
More informationMidterm Exam: March 19 Review Sheet handed out & on class website: Lecture notes & HW solutions also! Office Hours: Monday 11-2 and 3-4 PM
Today: Chapter. 12-Stars Midterm Exam: March 19 Review Sheet handed out & on class website: http://www.physics.sfsu.edu/~chris/astro115/ Lecture notes & HW solutions also! Office Hours: Monday 11-2 and
More informationAST 248, Lecture 2. James Lattimer. Department of Physics & Astronomy 449 ESS Bldg. Stony Brook University. January 28, 2015
AST 248, Lecture 2 James Lattimer Department of Physics & Astronomy 449 ESS Bldg. Stony Brook University January 28, 2015 The Search for Life in the Universe james.lattimer@stonybrook.edu Distances in
More informationLength. System of Units. System International (SI) Physics Department 1/21/2018. Phys1411 Goderya 1. Topics for Today s Class
PHYS 1403 Stars and Galaxies Topics for Today s Class 1. Measurements a) Measurements b) SI units c) Conversions Review from High School Math d) Scientific Notation e) Uncertainty 2. Chapter 1: Hear and
More informationPhys 100 Astronomy (Dr. Ilias Fernini) Review Questions for Chapter 1
Phys 100 Astronomy (Dr. Ilias Fernini) Review Questions for Chapter 1 MULTIPLE CHOICE (Right answers are reported in red) 1.. A solar system contains a. primarily planets. b. large amounts of gas and dust
More informationThe principle of geometrical parallax
The principle of geometrical parallax One of the hardest things to do in astronomy is to determine how far away things are. Does the star Vega in Lyra appear exceptionally bright because it s an intrinsically
More information9/5/16. Astronomy 1001 Syllabus Sec 1 T,Th AM; Sec 2 T,TH PM. Astronomy 1001 First Assignments: Chapter 1: A Modern View of the Universe
9/5/16 Astronomy 1001 Syllabus Sec 1 T,Th AM; Sec 2 T,TH PM Syllabus: http://www.astro.umn.edu/courses/1001/syllabi/ Lecture notes: http://www.astro.umn.edu/courses/1001/ lecnotes/ Exams: http://www.astro.umn.edu/courses/1001/
More informationStars, Galaxies & the Universe Announcements. Stars, Galaxies & the Universe Observing Highlights. Stars, Galaxies & the Universe Lecture Outline
Stars, Galaxies & the Universe Announcements HW#3 due Tuesday (Tomorrow) at 3 pm Lab Observing Trip Tues (9/28) & Thurs (9/30) First Exam next Wed. (9/22) in class - will post review sheet, practice exam
More information1 (a) Explain what is meant by a white dwarf when describing the evolution of a star [1]
1 (a) Explain what is meant by a white dwarf when describing the evolution of a star.... [1] (b) Antares is a red giant and one of the brightest stars in the night sky. The parallax angle for this star
More informationIntroduction to the Universe. What makes up the Universe?
Introduction to the Universe What makes up the Universe? Objects in the Universe Astrophysics is the science that tries to make sense of the universe by - describing the Universe (Astronomy) - understanding
More information