Midterm Exam: March 19 Review Sheet handed out & on class website: Lecture notes & HW solutions also! Office Hours: Monday 11-2 and 3-4 PM
|
|
- Marian Douglas
- 5 years ago
- Views:
Transcription
1 Today: Chapter. 12-Stars Midterm Exam: March 19 Review Sheet handed out & on class website: Lecture notes & HW solutions also! Office Hours: Monday 11-2 and 3-4 PM
2 Voting Question What happens every 11 years on the Sun? A.) The energy production increases B.) There is an eclipse C.) The number of sunspots increases D.) The light output decreases significantly
3 Voting Question The source of energy in the Sun is A.) The chemical burning of Hydrogen B.) The nuclear fusion of Hydrogen into Helium C.) Nuclear fission of Helium into Hydrogen D.) Nuclear fission of Uranium
4 Nuclear Power can be generated two ways: Fission Fusion! Breaking up a big nucleus, (like Uranium) to produce smaller nuclei (like Lead)! Combining small nuclei (like Hydrogen) to form larger (like Helium) Both types have been used by people here on Earth.
5 Nuclear Weapons First nuclear weapons were build by the U.S. during World War II Fission bombs, using Uranium & Plutonium, destroyed the cities of Hiroshima & Nagasaki at the end of the war. Since then, more powerful fusion bombs have been built (Hydrogen bombs) Trinity Test, New Mexico, 1945 First Nuclear Bomb Hydrogen (fusion) bomb, Pacific Ocean, 1962
6 Nuclear weapons testing contaminated Earth s atmosphere with radiation. So, in 1963, nations agreed not to explode them above ground. Nine countries have nuclear weapons, but US and Russia have the most (7,000 each)
7 America s nuclear weapons are managed by the Department of Energy. Dr. Stephen Chu, Fmr. US Energy Sec. Rick Perry, US Energy Secretary
8 Nuclear Energy Generation The energy of the Nucleus can also be used to generate electricity. Current, nuclear reactors use controlled fission, to do this, generating considerable nuclear waste, and (on rare occasions) melting down. Nuclear fusion reactors are still experimental...but may one day provide copious clean energy, with little waste. If we can figure out how to make controlled fusion, we will have a reliable, and clean source of energy. San Onofre Fission Plant, CA Tokamak, an experimental nuclear fusion reactor
9
10 Fusion powers every star
11 The Sun: Summary! Size & Mass! Interior: Core, Convection Zone! Atmosphere: Photosphere, Corona, Chromosphere! Sunspots: 11 year cycle.! Energy source: nuclear fusion of hydrogen to helium
12 Chapter 11: Stars Optional: 11:12-11:13
13 We already know how to determine a star s: surface temperature chemical composition motion Next, we will learn how we can determine its: distance brightness mass
14 Measuring the Distance to Stars! Measuring distances is difficult! However, several reliable methods can be used. The best method for measuring distances of nearby stars is called parallax. It relies on observing a star from two different places.
15 Field of background stars: Parallax test
16 Parallax Background Stars! We obtain a different perspective on a star by observing it at different times of the year. Nearby Star! The star is compared to distant background stars! In 6 months the Earth has moved 2 AU! The parallax method lets us measure the distance to stars that are closer than about 1000 light years away.
17 Measuring Distances: Parallax! The larger the star s distance, d, the smaller its parallax p.! So distance and parallax are inversely related.! d = 1 / p
18 Measuring Angles & Distances! Most stars have a parallax angle, p, which is very small!. much smaller than 1 degree.! So parallax angles are measured in units of arc seconds! 1/60 of one degree = 1 arc minute! 1 /60 of one arc minute = 1 arc second.! Distances to stars are measured in either: light years, or parsecs.! 1 parsec = 3.2 light years (parsec = PARallax of one arcsec)
19 Parallax Example! If a star has a parallax 1 arcsecond, then its distance is 1 parsec.! Suppose a star has a parallax 0.1 arc seconds! Question: what is its distance in parsecs?! Answer: d = 1 / p! d = 1 / 0.1! d = 10 parsecs = 32 light years.! (note: p = parallax angle, not parsecs)
20 Background Stars Parallax Measures Distance Parallax (p) is the angle a star appears to move by when Earth orbits the Sun. (p measured in arc seconds ) Nearby Star It tells us the distance (d) to the star: (d measured in parsecs ) p = 1/d
21 Discussion Question Three stars have different parallaxes: -Proxima s parallax is: 0.8 arc sec -Sirius parallax is: 0.4 arc sec -Polaris parallax is: arc sec Q1: Which Star is closest, which is farthest? Q2: Can you tell which star is brightest?
22 How Powerful Are the Stars?! Power is energy output per second.! Power is measured in Joules per second, or Watts! eg. a 100 Watt light bulb uses 100 Joules of energy per sec.! We measure the power, or brightness, of stars in 2 ways: luminosity and magnitude. The Luminosity (L) of a star is just its wattage. The Sun s luminosity is: L Sun = 380,000,000,000,000,000,000,000,000 = 3.8 x Watts! =380 Yottawatts! Other stars can be measured against the Sun.
23 Instead of Watts, we ll use the Sun s Luminosity (L SUN = ) to measure other stars. Luminosities of Different Stars! Our Sun: L = 1.0 L sun! Sirius: L = 25 Lsun! Polaris (North star): L = 1,300 Lsun! Proxima: L = L sun
24 The Most Luminous Star End S. 2 Star Eta Carinae and surrounding nebula! Eta Carinae is the most luminous star known.! L = 4 Million L sun!!!!! In ~5 seconds, it emits as much light as the Sun in 1 year!
25 Measuring Stars: Magnitudes Another way to measure the brightness of a star is its Magnitude Ancient people put stars into 5 classes, from First Magnitude (brightest) to Fifth Magnitude (dimmest) This system is still in use today
26 Magnitudes of stars in Orion
27 Magnitudes Lower magnitudes = brighter stars So a 1st magnitude star is brighter than a 2nd mag. star We use the symbol: m to mean magnitude. Originally there were only magnitudes 1-5 However a very bright object can even have a negative magnitude.
28 Magnitude Examples The planet Venus magnitude is m = -4.0 A very faint object can have a magnitude above 5. E.g.: A distant galaxy has a magnitude: m =20. Q: What object in the sky has the lowest magnitude?
How does the Sun shine? What is the Sun s structure? Lifetime of the Sun. Luminosity of the Sun. Radiation Zone. Core 3/30/17
What is the Sun s structure? From inside out, the layers are: Core Radiation Zone Convection Zone Photosphere Chromosphere Corona How does the Sun shine? The Sun has its own energy source Main difference
More informationConvection causes granules. Photosphere isn t actually smooth! Granules Up-Close: like boiling water. Corona or of the Sun. Chromosphere: sphere of
Overview Properties of the Sun Sun s outer layers Photosphere Chromosphere Corona Solar Activity Sunspots & the sunspot cycle Flares, prominences, CMEs, aurora Sun s Interior The Sun as an energy source
More informationHydrogen Lines. What can we learn from light? Spectral Classification. Visible Hydrogen Spectrum Lines: Series. Actual Spectrum from SDSS
What can we learn from light? Hydrogen Lines Temperature Energy Chemical Composition Speed towards or away from us All from the! Lower E, Lower f, λ Visible! Higher E, Higher f, λ Visible Hydrogen Spectrum
More informationAstronomy 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
More informationSun s Properties. Overview: The Sun. Composition of the Sun. Sun s Properties. The outer layers. Photosphere: Surface. Nearest.
Overview: The Sun Properties of the Sun Sun s outer layers Photosphere Chromosphere Corona Solar Activity Sunspots & the sunspot cycle Flares, prominences, CMEs, aurora Sun s Interior The Sun as an energy
More informationCorrection to Homework
Today: Chapter 10 Reading Next Week: Homework Due March 12 Midterm Exam: March 19 Correction to Homework #1: Diameter of eye: 2.5 cm #10: See Ch. 11 Office Hours Monday. 11AM -2 PM Help Sessions Available:
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 informationChapter 8: The Family of Stars
Chapter 8: The Family of Stars We already know how to determine a star s surface temperature chemical composition motion Next, we will learn how we can determine its distance luminosity radius mass Measuring
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 informationChapter 14 Lecture. Chapter 14: Our Star Pearson Education, Inc.
Chapter 14 Lecture Chapter 14: Our Star 14.1 A Closer Look at the Sun Our goals for learning: Why does the Sun shine? What is the Sun's structure? Why does the Sun shine? Is it on FIRE? Is it on FIRE?
More information14.1 A Closer Look at the Sun
14.1 A Closer Look at the Sun Our goals for learning: Why does the Sun shine? What is the Sun's structure? Why does the Sun shine? Is it on FIRE? Is it on FIRE? NO! Chemical energy content Luminosity ~
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 information10/17/ A Closer Look at the Sun. Chapter 11: Our Star. Why does the Sun shine? Lecture Outline
Lecture Outline 11.1 A Closer Look at the Sun Chapter 11: Our Star Our goals for learning: Why does the Sun shine? What is the Sun's structure? Why does the Sun shine? Is it on FIRE? Is it on FIRE? Chemical
More informationChapter 14 Our Star A Closer Look at the Sun. Why was the Sun s energy source a major mystery?
Chapter 14 Our Star 14.1 A Closer Look at the Sun Our goals for learning Why was the Sun s energy source a major mystery? Why does the Sun shine? What is the Sun s structure? Why was the Sun s energy source
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 informationASTR Midterm 1 Phil Armitage, Bruce Ferguson
ASTR 1120-001 Midterm 1 Phil Armitage, Bruce Ferguson FIRST MID-TERM EXAM FEBRUARY 16 th 2006: Closed books and notes, 1 hour. Please PRINT your name and student ID on the places provided on the scan sheet.
More informationChapter 14 Lecture. The Cosmic Perspective Seventh Edition. Our Star Pearson Education, Inc.
Chapter 14 Lecture The Cosmic Perspective Seventh Edition Our Star 14.1 A Closer Look at the Sun Our goals for learning: Why does the Sun shine? What is the Sun's structure? Why does the Sun shine? Is
More information10/18/ A Closer Look at the Sun. Chapter 11: Our Star. Why does the Sun shine? Lecture Outline
10/18/17 Lecture Outline 11.1 A Closer Look at the Sun Chapter 11: Our Star Our goals for learning: Why does the Sun shine? What is the Sun's structure? Why does the Sun shine? Is it on FIRE? Is it on
More informationObservational Astronomy - Lecture 8 Stars I - Distances, Magnitudes, Spectra, HR Diagram
Observational Astronomy - Lecture 8 Stars I - Distances, Magnitudes, Spectra, HR Diagram Craig Lage New York University - Department of Physics craig.lage@nyu.edu April 7, 2014 1 / 36 JPL Horizons Database.
More informationPHYS 160 Astronomy Take-home Test #4 Fall 2017
PHYS 160 Astronomy Take-home Test #4 Fall 2017 Instructions: This is a take-home test. The test period starts Monday 11/27/2017 at 2:10pm and ends at Wednesday 11/29/2017 at 1:10pm. The test must represent
More informationMeasuring 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
More informationCHAPTER 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
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 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 informationChapter 14 Our Star Pearson Education, Inc.
Chapter 14 Our Star Basic Types of Energy Kinetic (motion) Radiative (light) Potential (stored) Energy can change type, but cannot be created or destroyed. Thermal Energy: the collective kinetic energy
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 informationMeasuring 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
More informationReading and Announcements. Read Chapters 9.5, 9.6, and 11.4 Quiz #4, Thursday, March 7 Homework #5 due Tuesday, March 19
Reading and Announcements Read Chapters 9.5, 9.6, and 11.4 Quiz #4, Thursday, March 7 Homework #5 due Tuesday, March 19 Stars The stars are distant and unobtrusive, but bright and enduring as our fairest
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 informationCASE STUDY FOR USE WITH SECTION B
GCE A level 325/0-A PHYSICS PH5 Assessment Unit CASE STUDY FOR USE WITH SECTION B Pre-Release Material To be opened on receipt A new copy of this Case Study will be given out in the examination 325 0A00
More informationTypes 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
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 informationThe Sun. the main show in the solar system. 99.8% of the mass % of the energy. Homework due next time - will count best 5 of 6
The Sun the main show in the solar system 99.8% of the mass 99.9999...% of the energy 2007 Pearson Education Inc., publishing as Pearson Addison-Wesley Homework due next time - will count best 5 of 6 The
More informationASTRONOMY 1 EXAM 3 a Name
ASTRONOMY 1 EXAM 3 a Name Identify Terms - Matching (20 @ 1 point each = 20 pts.) Multiple Choice (25 @ 2 points each = 50 pts.) Essays (choose 3 of 4 @ 10 points each = 30 pt 1.Luminosity D 8.White dwarf
More informationAy 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
More informationProton-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
More information18. 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
More informationHomework 2 AST 301, Sections and 46850, Spring NAME Student EID Score: on last page. Due Tuesday, March 1, 2016
Homework 2 AST 301, Sections 46845 and 46850, Spring 2016 NAME Student EID Score: on last page Due Tuesday, March 1, 2016 Questions A C should help you to understand the properties of light. Show your
More informationAstronomy 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.
More informationPhysical Data Mass = 2x10 30 kg (333,000 time more massive than the Earth) Diameter: 7x10 5 km (about 100 Earth radii) Volume: you can fit about 1.3 m
The Sun Physical Data Mass = 2x10 30 kg (333,000 time more massive than the Earth) Diameter: 7x10 5 km (about 100 Earth radii) Volume: you can fit about 1.3 million earths inside the sun! 70% Hydrogen,
More informationScience Period. Astronomy Unit PracticeTest 2014 Sci 7
Name: Date: Science Period Astronomy Unit PracticeTest 2014 Sci 7 Directions: Write the letter of the BEST answer on the appropriate space on the answer sheet. 2 points each 1.The model in which SUN is
More informationλ = 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.
More informationThe 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
More informationdays 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
More informationWelcome to Environmental Science!!!
Welcome to Environmental Science!!! The Sun Physical Data Mass = 2x10 30 kg (333,000 time more massive than the Earth) Diameter: 7x10 5 km (about 100 Earth radii) Volume: you can fit about 1.3 million
More informationGalaxies 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
More informationToday The Sun. Events
Today The Sun Events Last class! Homework due now - will count best 5 of 6 Final exam Dec. 20 @ 12:00 noon here Review this Course! www.case.edu/utech/course-evaluations/ The Sun the main show in the solar
More informationChapter 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
More informationStar Magnitudes & Distances with Stellarium (Stellarium Exercise #2)
Name Date Star Magnitudes & Distances with Stellarium (Stellarium Exercise #2) Millions of stars are scattered across the sky. Astronomers want to study these stars as carefully as possible. This means
More informationStars and Galaxies. Content Outline for Teaching
Section 1 Stars A. Patterns of stars - constellations 1. Ancient cultures used mythology or everyday items to name constellations 2. Modern astronomy studies 88 constellations 3. Some constellations are
More informationChapter 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
More information1 A Solar System Is Born
CHAPTER 16 1 A Solar System Is Born SECTION Our Solar System California Science Standards 8.2.g, 8.4.b, 8.4.c, 8.4.d BEFORE YOU READ After you read this section, you should be able to answer these questions:
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 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 informationCHAPTER 9: STARS AND GALAXIES
CHAPTER 9: STARS AND GALAXIES Characteristics of the Sun 1. The Sun is located about 150 million kilometres from the Earth. 2. The Sun is made up of hot gases, mostly hydrogen and helium. 3. The size of
More informationTextbook Chapters 24 - Stars Textbook Chapter 25 - Universe. Regents Earth Science with Ms. Connery
Textbook Chapters 24 - Stars Textbook Chapter 25 - Universe Regents Earth Science with Ms. Connery SPECTROSCOPY is the study of light. Read to learn - textbook pages 674-677 STAR LIGHT gives us characteristics
More information27.1: Characteristics of Stars
27.1: Characteristics of Stars STAR NOTES: Part 1 What is a Star? A body of gases that gives off energy in the form of light and heat. 27.1: Characteristics of Stars Are all stars the same? No 1. Stars
More informationL = 4 d 2 B p. 4. Which of the letters at right corresponds roughly to where one would find a red giant star on the Hertzsprung-Russell diagram?
Fall 2016 Astronomy - Test 3 Test form B Name Do not forget to write your name and fill in the bubbles with your student number, and fill in test form B on the answer sheet. Write your name above as well.
More informationL = 4 d 2 B p. 1. Which outer layer of the Sun has the highest temperature? A) Photosphere B) Corona C) Chromosphere D) Exosphere E) Thermosphere
Fall 2016 Astronomy - Test 3 Test form A Name Do not forget to write your name and fill in the bubbles with your student number, and fill in test form A on the answer sheet. Write your name above as well.
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 informationExam #2 Review Sheet. Part #1 Clicker Questions
Exam #2 Review Sheet Part #1 Clicker Questions 1) The energy of a photon emitted by thermonuclear processes in the core of the Sun takes thousands or even millions of years to emerge from the surface because
More informationCONTENT EXPECTATIONS
THE SUN & THE STARS CONTENT EXPECTATIONS STARS What are stars? Are they all the same? What makes them different? What is our nearest star? THE SUN Why is it important? provides heat and light that we need
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 informationMULTIPLE 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
More informationAstronomy Student Notes Name Our Sun and Other Stars Date Period
Astronomy Student Notes Our Sun and Other Stars Name Date Period Vocabulary: Please number and define each term below in a complete sentence on a separate sheet of paper(terms that have an *, please illustrate)
More informationEarth Science Lesson Plan Quarter 4, Week 7, Day 1
Earth Science Lesson Plan Quarter 4, Week 7, Day 1 Outcomes for Today Standard Focus: Earth Sciences 1.e Students know the Sun is typical star and is powered by nuclear reactions, primarily the fusion
More informationStars 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 -
More informationPHY2083 ASTRONOMY. Dr. Rubina Kotak Office F016. Dr. Chris Watson Office S036
PHY2083 ASTRONOMY Dr. Rubina Kotak r.kotak@qub.ac.uk Office F016 Dr. Chris Watson c.a.watson@qub.ac.uk Office S036 PHY2083 ASTRONOMY Weeks 1-6: Monday 10:00 DBB 0G.005 Wednesday 9:00 PFC 02/018 Friday
More informationHow the Sun Works. Presented by the
How the Sun Works Presented by the The Sun warms our planet every day, provides the light by which we see and is absolutely necessary for life on Earth. In this presentation, we will examine the fascinating
More informationStars, 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
More informationAST 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
More informationStars & Galaxies. Chapter 27, Section 1. Composition & Temperature. Chapter 27 Modern Earth Science Characteristics of Stars
Stars & Galaxies Chapter 27 Modern Earth Science Chapter 27, Section 1 27.1 Characteristics of Stars Composition & Temperature Scientists use the following tools to study stars Telescope Observation Spectral
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 informationHW 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
More informationThe Electromagnetic Spectrum
The Electromagnetic Spectrum Three Kinds of Spectra Sun: The Nearest Star Radius 696,000 km 109 Re Mass 2 x 10^30 kg 300,000 Me Density 1400 kg/m^3 Luminosity 3.8x10^26 Watts (board calc.) Comp. 70% H,
More informationINSIDE LAB 8: Plotting Stars on the Hertzsprung- Russell Diagram
INSIDE LAB 8: Plotting Stars on the Hertzsprung- Russell Diagram OBJECTIVE: To become familiar with the Hertzsprung-Russell diagram and the method of spectroscopic parallax. DISCUSSION: The Hertzsprung-Russell
More informationChapter 8 The Sun Our Star
Note that the following lectures include animations and PowerPoint effects such as fly ins and transitions that require you to be in PowerPoint's Slide Show mode (presentation mode). Chapter 8 The Sun
More informationChapter Introduction Lesson 1 The View from Earth Lesson 2 The Sun and Other Stars Lesson 3 Evolution of Stars Lesson 4 Galaxies and the Universe
Chapter Introduction Lesson 1 The View from Earth Lesson 2 The Sun and Other Stars Lesson 3 Evolution of Stars Lesson 4 Galaxies and the Universe Chapter Wrap-Up What makes up the universe and how does
More informationNSB ideas on Hertzsprung-Russell diagram
Contents Big ideas Not so big ideas about the sun Not so big ideas about Hertzsprung-Russell diagram Not so big ideas about white dwarfs, neutron stars, and black holes Questions on chapter 10, 11, 12,
More informationA Closer Look at the Sun
Our Star A Closer Look at the Sun Our goals for learning Why was the Sun s energy source a major mystery? Why does the Sun shine? What is the Sun s structure? Why was the Sun s energy source a major mystery?
More informationFacts About The Sun. The Sun is a star found at the of the Solar System. It makes up around % of the Solar System s mass.
Facts About is a star found at the of the Solar System. It makes up around % of the Solar System s mass. At around 1,392,000 kilometres (865,000 miles) wide, the Sun s is about 110 times wider than Earth
More informationUniverse Review. 3. The light emitted from a star is studied by astronomers to determine which of the following properties?
Name: Universe Review Period: 1. Which type of telescope uses mirrors to focus visible light? A. reflecting telescope B. radio telescope C. infrared telescope D. refracting telescope 2. Which type of telescope
More informationChapter 12: The Life Cycle of Stars (contʼd) How are stars born, and how do they die? 4/9/09 Habbal Astro Lecture 25 1
Chapter 12: The Life Cycle of Stars (contʼd) How are stars born, and how do they die? 4/9/09 Habbal Astro 110-01 Lecture 25 1 12.3 Life as a High-Mass Star Learning Goals What are the life stages of a
More informationStars & Galaxies. Chapter 27 Modern Earth Science
Stars & Galaxies Chapter 27 Modern Earth Science Chapter 27, Section 1 27.1 Characteristics of Stars How do astronomers determine the composition and surface temperature of a star? Composition & Temperature
More informationProperties of Stars. 1.1 Brightnesses of Stars
Properties of Stars 1.1 Brightnesses of Stars I m sure you have noticed that some stars are very bright, others less bright, and some are quite dim. There is a true brightness of a star and an apparent
More informationMagnitudes. How Powerful Are the Stars? Luminosities of Different Stars
How Powerful Are the Stars? Some stars are more powerful than others Power is energy output per. (Example: 00 Watts = 00 joules per second) Astronomers measure the power, or brightness of stars in ways:
More informationMatter and Energy. Previous studies have taught us that matter and energy cannot be created nor destroyed We balance equations to obey this law.
Fission & Fusion Matter and Energy Previous studies have taught us that matter and energy cannot be created nor destroyed We balance equations to obey this law. 2 H 2 O 2 H 2 + O 2 We now need to understand
More informationStellar 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.
More informationAnnouncements. - Homework #5 due today - Review on Monday 3:30 4:15pm in RH103 - Test #2 next Tuesday, Oct 11
Announcements - Homework #5 due today - Review on Monday 3:30 4:15pm in RH103 - Test #2 next Tuesday, Oct 11 Review for Test #2 Oct 11 Topics: The Solar System and its Formation The Earth and our Moon
More informationThe Sun Our Star. Properties Interior Atmosphere Photosphere Chromosphere Corona Magnetism Sunspots Solar Cycles Active Sun
The Sun Our Star Properties Interior Atmosphere Photosphere Chromosphere Corona Magnetism Sunspots Solar Cycles Active Sun General Properties Not a large star, but larger than most Spectral type G2 It
More information1 A= one Angstrom = 1 10 cm
Our Star : The Sun )Chapter 10) The sun is hot fireball of gas. We observe its outer surface called the photosphere: We determine the temperature of the photosphere by measuring its spectrum: The peak
More information! Exam 1 in this classroom in 1 week (Oct 1 st )! 40 Multiple choice questions! Will cover material up to and including today.!
This Class (Lecture 12): Why does the Sun Shine? Next Class: Why is the Sun Yellow? HW5 due Monday Exam 1 next Friday!! Exam 1 in this classroom in 1 week (Oct 1 st )! 40 Multiple choice questions! Will
More informationA100 Exploring the Universe: How Stars Work. Martin D. Weinberg UMass Astronomy
A100 Exploring the Universe: How Stars Work Martin D. Weinberg UMass Astronomy astron100-mdw@courses.umass.edu October 07, 2014 Read: Chaps 14, 15 10/07/12 slide 1 Exam scores posted in Mastering Questions
More informationOur sole source of light and heat in the solar system. A very common star: a glowing g ball of gas held together by its own gravity and powered
The Sun Visible Image of the Sun Our sole source of light and heat in the solar system A very common star: a glowing g ball of gas held together by its own gravity and powered by nuclear fusion at its
More informationChapter 9: Measuring the Stars
Chapter 9: Measuring the Stars About 10 11 (100,000,000,000) stars in a galaxy; also about 10 11 galaxies in the universe Stars have various major characteristics, the majority of which fall into several
More informationFission & Fusion Movie
Fission & Fusion Movie Matter and Energy Previous studies have taught us that matter and energy cannot be created nor destroyed We balance equations to obey this law. 2 H 2 O 2 H 2 + O 2 We now need to
More informationChapter 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:
More informationMeasuring stellar distances.
Measuring stellar distances This method can be used to measure distances up to 100pc Some new technology allows measuring distances up to 200pc using this method p= 1/d Stellar Parallax.htm This method
More informationForces and Nuclear Processes
Forces and Nuclear Processes To understand how stars generate the enormous amounts of light they produce will require us to delve into a wee bit of physics. First we will examine the forces that act at
More informationChapter 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
More information