Test Ques4ons. Median Grade: 82/100 High Score: 99/100
|
|
|
- Emil Davidson
- 5 years ago
- Views:
Transcription
1 Day 11: Stars Review of Test Ar4cle Sharing Reading/Mastering Astronomy Ques4ons Lecture on Spectral Type Break Lecture on Hertzsprung- Russell Diagram L- T: H- R Diagram, p 117 Summary
2 Test Ques4ons Median Grade: 82/100 High Score: 99/100
3 Did the midterm do a good job of tes4ng informa4on we emphasized in class? A. Very much so either I knew the informa4on or I should have known it B. PreVy good it seemed fairly appropriate to the class C. Somewhat some of the ques4ons were out of ley field but it mostly worked D. Not so much some of it I recognized but a lot I can t remember covering E. (all colors) Not at all. What were you thinking?
4 Ar4cle Review
5
6 Atmosphere of Star
7 Atmosphere of Star
8 Absorp4on Spectra
9
10 Cecilia Payne- Gaposchkin
11
12 Which Hydrogen Atom will not produce absorp4on lines? A. Hydrogen atom with one electron in ground energy level B. Hydrogen atom with one electron in second energy level C. Hydrogen atom with two electrons, one in ground energy level and one in second energy level D. Ionized hydrogen (Hydrogen atom with no electrons)
13 Which Hydrogen Atom will not produce absorp4on lines? A. Hydrogen atom with one electron in ground energy level B. Hydrogen atom with one electron in second energy level C. Hydrogen atom with two electrons, one in ground energy level and one in second energy level D. Ionized hydrogen (Hydrogen atom with no electrons)
14 What type of hydrogen gas is least likely to produce absorp4on lines? A. Extremely hot hydrogen gas B. Warm hydrogen gas C. Cold hydrogen gas D. Hydrogen gas in a strong magne4c field
15 What type of hydrogen gas is least likely to produce absorp4on lines? A. Extremely hot hydrogen gas B. Warm hydrogen gas C. Cold hydrogen gas D. Hydrogen gas in a strong magne4c field
16 Hydrogen is ionized Hydrogen is not ionized. Many electrons in 2 nd energy level Hydrogen is not ionized. All electrons in ground energy level
17 Hydrogen lines in visible part of the spectrum are produced by atoms star4ng at the second energy level
18 What gas will produce the most hydrogen absorp4on lines in the visible part of the spectrum? A. Extremely hot gas: all hydrogen is ionized B. Fairly hot gas: all hydrogen electrons in very high energy levels C. Warm gas: many hydrogen electrons in second energy level D. Cold gas: all hydrogen electrons in ground energy level
19 What gas will produce the most hydrogen absorp4on lines in the visible part of the spectrum? A. Extremely hot gas: all hydrogen is ionized B. Fairly hot gas: all hydrogen electrons in very high energy levels C. Warm gas: many hydrogen electrons in second energy level D. Cold gas: all hydrogen electrons in ground energy level
20 Hydrogen is ionized Hydrogen is not ionized. Many electrons in 2 nd energy level Hydrogen is not ionized. All electrons in ground energy level
21 Spectral Type Oh Be Fine Girl/Guy Kiss Me
22 Stellar Absorp4on Lines Require gas of a certain element of just the right temperature to be produced Too hot, and the gas of that element is ionized Too cold, and electrons are all in ground level so they can only produce lines for energy transi4ons star4ng at ground We can, therefore, use lines to tell us stellar temperatures
23 Break
24
25 Income vs. Mass
26 Hertzsprung- Russell Diagram Luminosity Surface Temperature
27 Hertzsprung- Russell Diagram
28 Hertzsprung- Russell Diagram
29 Hertzsprung- Russell Diagram
30 Hertzsprung- Russell Diagram
31 Hertzsprung- Russell Diagram Magnitudes
32 L- T: H- R Diagram, page 117
33 Hertzsprung- Russell Diagram
34 The stars Antares and Mima each have the same luminosity. Antares is cooler than Mima. Which star is larger? A. Antares B. Mima C. Both stars are the same size D. There is insufficient informa4on to determine this
35 The stars Antares and Mima each have the same luminosity. Antares is cooler than Mima. Which star is larger? A. Antares B. Mima C. Both stars are the same size D. There is insufficient informa4on to determine this
36 The stars Antares and Mima each have the same luminosity. Antares is cooler than Mima. Which star is larger?
37 Size Luminosity Temperature
38 Rigel is much more luminous than Sirius B. Rigel and Sirius B have the same temperature. Which star has A. Rigel B. Sirius B the greater surface area? C. The have the same surface area D. There is insufficient informa4on to answer this ques4on
39 Rigel is much more luminous than Sirius B. Rigel and Sirius B have the same temperature. Which star has A. Rigel B. Sirius B the greater surface area? C. The have the same surface area D. There is insufficient informa4on to answer this ques4on
40 Rigel is much more luminous than Sirius B. Rigel and Sirius B have the same temperature. Which star has the greater surface area?
41 Size Luminosity Temperature
42 Main Sequence: Hydrogen Burning Luminosity Temperature
43 Giants/Supergiants: Dying Stars Luminosity Temperature
44 White Dwarfs: Dead Stars Luminosity Temperature
45 Lalande is a nearby star half the mass of the Sun. It is in gravita4onal equilibrium (i.e., it is neither expanding nor contrac4ng). What force supports Lalande and keeps it from collapsing in on itself? What force binds Lalande together and keeps it from exploding outward? How does the strength of this force for Lalande compare to the strength of this same force for the Sun? What is the net force this star is experiencing? How does the temperature at the center of Lalande compare to the temperature at the center of the Sun? How does the rate of fusion at the center of Lalande compare to the rate of fusion at the center of the Sun?
46 Hertzsprung- Russell Diagram
47
48 Different Mass Main Sequence Low Mass High Mass (0.1 Solar Mass) (50 Solar Masses) Dim (0.001 Solar Luminosity) Cool (3000 K) Red Small (0.1 Solar Radius) Long- lived (100 Billion years) Bright (1 Million Solar Luminosity) Hot (30,000 K) Blue Large (10 Solar Radii) Short- Lived (10 Million years)
49 Summary Absorp4on line spectra and peak wavelength tell us stellar temperature Absorp4on lines depend on the type of gas available in the stellar atmosphere Stars can be sorted by temperature/stellar type: O, B, A, F, G, K, M The Hertzsprung- Russell diagram shows stars divided into Main Sequence, Giants, and White dwarfs Higher mass stars are hover, bigger, and short lived
50 Homework LT: H- R Diagram Reading: Ch and 16.2 (p ) MasteringAstronomy: Star Forma4on
Properties of Stars & H-R Diagram
Properties of Stars & H-R Diagram What is a star? A cloud of gas, mainly hydrogen and helium The core is so hot/dense that nuclear fusion can occur. The fusion converts light nuclei (elements) into heavier
Stars: some basic characteristics
Stars: some basic characteristics Stars! How bright are they? How massive are they? What are the different types? How long do they live? How hot are they? Stellar brightness and luminosity The apparent
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
Family of stars. Fred Sarazin Physics Department, Colorado School of Mines. PHGN324: Family of stars
Family of stars Reminder: the stellar magnitude scale In the 1900 s, the magnitude scale was defined as follows: a difference of 5 in magnitude corresponds to a change of a factor 100 in brightness. Dm
Summary of Stellar Proper/es
Summary of Stellar Proper/es Large range of Stellar Luminosi/es: 10 4 to 10 6 L sun Large range of Stellar Radii: 10 2 to 10 3 R sun Modest range of Stellar Temperatures: 3000 to >50,000 K Wide Range of
Announcements. Lecture 11 Properties of Stars. App Bright = L / 4!d 2
Announcements Quiz#3 today at the end of 60min lecture. Homework#3 will be handed out on Thursday. Due October 14 (next Thursday) Review of Mid-term exam will be handed out next Tuesday. Mid-term exam
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
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
The Life Histories of Stars I. Birth and Violent Lives
The Life Histories of Stars I Birth and Violent Lives Stellar evolution--first problem for new discipline of astrophysics What is a star? What is it made of? How does it produce and release energy? How
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
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
Teacher of the Week DEVIL PHYSICS THE BADDEST CLASS ON CAMPUS IB PHYSICS
Teacher of the Week DEVIL PHYSICS THE BADDEST CLASS ON CAMPUS IB PHYSICS TSOKOS LESSON E-2 STELLAR RADIATION IB Assessment Statements Topic E-2, Stellar Radiation and Stellar Types Energy Source E.2.1.
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
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
Stars III The Hertzsprung-Russell Diagram
Stars III The Hertzsprung-Russell Diagram Attendance Quiz Are you here today? (a) yes Here! (b) no (c) here is such a 90 s concept Today s Topics (first half) Spectral sequence and spectral types Spectral
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
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 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:
Astronomy 210. Outline. Stellar Properties. The Mosquito Dilemma. Solar Observing & HW9 due April 15 th Stardial 2 is available.
Astronomy 210 Outline This Class (Lecture 31): Stars: Spectra and the H-R Diagram Next Class: Life and Death of the Sun Solar Observing & HW9 due April 15 th Stardial 2 is available. The Mosquito dilemma
Lecture 10: The Hertzsprung-Russell Diagram Reading: Sections
Lecture 10: The Hertzsprung-Russell Diagram Reading: Sections 19.7-19.8 Key Ideas The Hertzsprung-Russell (H-R) Diagram Plot of Luminosity vs. Temperature for stars Features: Main Sequence Giant & Supergiant
Day 13: Low- mass Star Evolu5on
Day 13: Low- mass Star Evolu5on Reading and MasteringAstronomy Ques5ons Review of star forma5on and degeneracy pressure LT: Star Forma5on and Life5mes Mini- lecture: Low- mass star evolu5on Break Mini-
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
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
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
Stellar Evolution and the HertzsprungRussell Diagram 7/14/09. Astronomy 101
Stellar Evolution and the HertzsprungRussell Diagram 7/14/09 Astronomy 101 Astronomy Picture of the Day Astronomy 101 Outline for Today Astronomy Picture of the Day News Articles Business Return Lab 5
Lecture 11: The Internal Structure of Stars Reading: Section 18-2
Lecture 11: The Internal Structure of Stars Reading: Section 18-2 Key Ideas: Observational Clues to Stellar Structure H-R Diagram Mass-Luminosity Relation Hydrostatic Equilibrium Balance between Gravity
Selected Questions from Minute Papers. Outline - March 2, Stellar Properties. Stellar Properties Recap. Stellar properties recap
Black Holes: Selected Questions from Minute Papers Will all the material in the Milky Way eventually be sucked into the BH at the center? Does the star that gives up mass to a BH eventually get pulled
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
Chapter 6. Atoms and Starlight
Chapter 6 Atoms and Starlight What is light? Light is an electromagnetic wave. Wavelength and Frequency wavelength frequency = speed of light = constant Particles of Light Particles of light are called
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
Stars and HR Diagrams
Stars and HR Diagrams Elements are not Elementary: the Building Blocks of Nature Atoms are made from protons, neutrons, electrons Chemical elements are named by the number A of protons in their nucleus
Stars: Intro & Classification
Stars: Intro & Classification Astronomy 1 Elementary Astronomy LA Mission College Spring F2015 Quotes & Cartoon of the Day The wonder is, not that the field of stars of so vast, but that man has measured
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
Remember from Stefan-Boltzmann that 4 2 4
Lecture 17 Review Most stars lie on the Main sequence of an H&R diagram including the Sun, Sirius, Procyon, Spica, and Proxima Centauri. This figure is a plot of logl versus logt. The main sequence is
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
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
Stars. The composition of the star It s temperature It s lifespan
Stars Stars A star is a ball of different elements in the form of gases The elements and gases give off electromagnetic radiation (from nuclear fusion) in the form of light Scientists study the light coming
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
HR Diagram Student Guide
Name: HR Diagram Student Guide Pretest Score: Background Information Work through the background sections on Spectral Classification, Luminosity, and the Hertzsprung-Russell Diagram. Then complete the
ASTRONOMY QUIZ NUMBER 11
ASTRONOMY QUIZ NUMBER. Suppose you measure the parallax of a star and find 0. arsecond. The distance to this star is A) 0 light-years B) 0 parsecs C) 0. light-year D) 0. parsec 2. A star is moving toward
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
What did you think of Exam 1? ! Dates: a)! Too easy b)! Too hard c)! Just right d)! A little easy e)! A little hard
! Good job!! Average = 83.3! Median = 84 This Class (Lecture 15): The Dying Sun Micro-meteorite lab due tonight! Next Class: Killer Sun HW 6 due next Monday. Music: Why Does the Sun Really Shine They Might
Magnitudes. 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:
! 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
Temperature, Blackbodies & Basic Spectral Characteristics.
Temperature, Blackbodies & Basic Spectral Characteristics. Things that have one primary temperature but also exhibit a range of temperatures are known in physics as blackbodies. They radiate energy thermally.
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)
Chapter 8: The Family of Stars
Chapter 8: The Family of Stars Motivation We already know how to determine a star s surface temperature chemical composition surface density In this chapter, we will learn how we can determine its distance
LAB: Star Classification
Name: LAB: Star Classification INTRODUCTION: Like most scientists, astronomers like to categorize the Universe around them, and stars are no exception. Here s how astronomers classify stars into different
L = 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.
L = 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.
The H-R Diagram. Image credit: NOAO
The H-R Diagram Image credit: NOAO Luminosity, Temperature, Radius Recall: apparent magnitude, absolute magnitude, and distance are related. We now have a method for finding the luminosity and a method
Hertzprung-Russel and colormagnitude. ASTR320 Wednesday January 31, 2018
Hertzprung-Russel and colormagnitude diagrams ASTR320 Wednesday January 31, 2018 H-R diagram vs. Color- Magnitude Diagram (CMD) H-R diagram: Plot of Luminosity vs. Temperature CMD: Plot of magnitude vs.
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
Review Questions for the new topics that will be on the Final Exam
Review Questions for the new topics that will be on the Final Exam Be sure to review the lecture-tutorials and the material we covered on the first three exams. How does speed differ from velocity? Give
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
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
Low-mass Stellar Evolution
Low-mass Stellar Evolution The lives of low-mass stars And the lives of massive stars The Structure of the Sun Let s review: The Sun is held together by? The inward force is balanced by? Thinking about
The Physics of Light, part 2. Astronomy 111
Lecture 7: The Physics of Light, part 2 Astronomy 111 Spectra Twinkle, twinkle, little star, How I wonder what you are. Every type of atom, ion, and molecule has a unique spectrum Ion: an atom with electrons
Astronomy-part 3 notes Properties of Stars
Astronomy-part 3 notes Properties of Stars What are Stars? Hot balls of that shine because nuclear fusion (hydrogen to helium) is happening at their cores. They create their own. Have different which allow
Chapter 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
Astr 2320 Tues. March 7, 2017 Today s Topics
Astr 2320 Tues. March 7, 2017 Today s Topics Chapter 13: Stars: Binary Stars Determination of Stellar Properties vi Binary Stars Classification of Binary Stars Visual Binaries Both stars visible Only one
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
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
The Amazing Power of Starlight
The Amazing Power of Starlight Chapter 6 Just by analyzing the light received from a star, astronomers can retrieve information about a star s Starlight and Atoms 1. Total energy output 2. Surface temperature
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
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
Chapter 15 Reading Quiz Clickers. The Cosmic Perspective Seventh Edition. Surveying the Stars Pearson Education, Inc.
Reading Quiz Clickers The Cosmic Perspective Seventh Edition Surveying the Stars 15.1 Properties of Stars How do we measure stellar luminosities? How do we measure stellar temperatures? How do we measure
Stellar Evolution. The lives of low-mass stars. And the lives of massive stars
Stellar Evolution The lives of low-mass stars And the lives of massive stars The Structure of the Sun Let s review: The Sun is held together by what force? The inward force is balanced by what other force?
Fusion in first few minutes after Big Bang form lightest elements
Fusion in first few minutes after Big Bang form lightest elements Stars build the rest of the elements up to Iron (Fe) through fusion The rest of the elements beyond Iron (Fe) are produced in the dying
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?
NSCI 314 LIFE IN THE COSMOS
NSCI 314 LIFE IN THE COSMOS 2 BASIC ASTRONOMY, AND STARS AND THEIR EVOLUTION Dr. Karen Kolehmainen Department of Physics CSUSB COURSE WEBPAGE: http://physics.csusb.edu/~karen MOTIONS IN THE SOLAR SYSTEM
Stars & 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
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 =
Astronomy 10 Test #2 Practice Version
Given (a.k.a. `First ) Name(s): Family (a.k.a. `Last ) name: ON YOUR PARSCORE: `Bubble your name, your student I.D. number, and your multiple-choice answers. I will keep the Parscore forms. ON THIS TEST
ASTRONOMY 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
Homework 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
Lecture 16: The life of a low-mass star. Astronomy 111 Monday October 23, 2017
Lecture 16: The life of a low-mass star Astronomy 111 Monday October 23, 2017 Reminders Online homework #8 due Monday at 3pm Exam #2: Monday, 6 November 2017 The Main Sequence ASTR111 Lecture 16 Main sequence
Summer 2013 Astronomy - Test 3 Test form A. Name
Summer 2013 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
the nature of the universe, galaxies, and stars can be determined by observations over time by using telescopes
the nature of the universe, galaxies, and stars can be determined by observations over time by using telescopes The spectral lines of stars tell us their approximate composition Remember last year in Physics?
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
Homework 9. Quiz Instruc!ons. Question 1. Question 2. 1 pts. 1 pts. ! This is a preview of the draft version of the quiz. Started: Mar 29 at 9:24pm
Homework 9! This is a preview of the draft version of the quiz Started: Mar 29 at 9:24pm Quiz Instruc!ons Question 1 The Sun's spectrum peaks in the yellow-green region of optical light. The Main Sequence
Stellar Nucleosynthesis
Stellar Nucleosynthesis What makes the sun shine? Gravita7onal contrac7on Chemical reac7ons Nucleosynthesis Stellar Nucleosynthesis The PP chain The CNO cycle The Triple alpha process and on to Fe Stellar
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
The Hertzsprung - Russell Diagram Laboratory 11
The Hertzsprung - Russell Diagram Laboratory 11 Objective: In this laboratory a random sample of stars will be used to create a HR Diagram. From the diagram it will be determined which category certain
To infinity, and beyond!
stars The night sky is filled with stars that shine at different levels of brightness. The brightness of the stars we observe can be related to the size of the star or its distance from Earth. In order
Stuff to do 10/4/18. Topics for Today. ASTR 1040: Stars & Galaxies
ASTR 1040: Stars & Galaxies Etched Hourglass Nebula Prof. Juri Toomre TAs: Ryan Horton.Loren Matilsky Lecture 12 Thur 4 Oct 2018 zeus.colorado.edu/astr1040-toomre Stuff to do Paper shuffle: Homework #5
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
Exam 1 will cover. The Day of the Exam. Astronomy Picture of the Day: Today s Class: Measuring temperatures of stars
September 25, 2013 Reading: Chapter 15, section 15.1. Exam 1 next class! Review Session tomorrow night, Sep. 26, at 7 pm in Duane G2B47. Naked eye observing session tonight at 8 pm. Volunteers for Astronomy
Masses are much harder than distance, luminosity, or temperature. Binary Stars to the Rescue!! AST 101 Introduction to Astronomy: Stars & Galaxies
Last Two Classes Measuring the Stars AST 101 Introduction to Astronomy: Stars & Galaxies 1. Measuring distances 2. Measuring stellar luminosities 3. Measuring temperatures Next 4. Measuring masses Masses
Calculating Main Sequence Lifetimes
Calculating Main Sequence ifetimes At the beginning of the twentieth century two astronomers, the Danish E. Hertzsprung and the American H. N. Russell, established a correlation between two important stellar
Astronomy Ch. 20 Stellar Evolution. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Name: Period: Date: Astronomy Ch. 20 Stellar Evolution MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) A star (no matter what its mass) spends
Astronomy Ch. 20 Stellar Evolution. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Name: Period: Date: Astronomy Ch. 20 Stellar Evolution MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) A star (no matter what its mass) spends
Exam #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
CONTENT 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
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
Deducing Temperatures and Luminosities of Stars (and other objects ) Electromagnetic Fields. Sinusoidal Fields
Deducing Temperatures and Luminosities of Stars (and other objects ) Review: Electromagnetic Radiation Gamma Rays X Rays Ultraviolet (UV) Visible Light Infrared (IR) Increasing energy Microwaves Radio
Lecture 14: Studying the stars. Astronomy 111 Monday October 16, 2017
Lecture 14: Studying the stars Astronomy 111 Monday October 16, 2017 Reminders Homework #7 due Monday I will give a lecture on DES and LIGO tomorrow at 4pm in the Mitchell Institute Studying the stars
Star Formation A cloud of gas and dust, called a nebula, begins spinning & heating up. Eventually, it gets hot enough for fusion to take place, and a
Stars Star- large ball of gas held together by gravity that produces tremendous amounts of energy and shines Sun- our closest star Star Formation A cloud of gas and dust, called a nebula, begins spinning
Astronomical Study: A Multi-Perspective Approach
Astronomical Study: A Multi-Perspective Approach Overview of Stars Motion Distances Physical Properties Spectral Properties Magnitudes Luminosity class Spectral trends Binary stars and getting masses Stellar