Beer, Bureaucracy and Binary Stars

Size: px
Start display at page:

Download "Beer, Bureaucracy and Binary Stars"

Transcription

1 Beer, Bureaucracy and Binary Stars Robert Izzard AIfA, Bonn

2 Orbital Dynamics BINARY STARS Convection Mixing Fluid Transfer Tides Winds Robert Izzard, Argelander Institute for Astronomy, University of Bonn

3 A (typical?) Stellar System Robert Izzard (AIfA, Bonn) Beer, Bureaucracy and Binary Stars 3 / 17

4 A Binary Stellar System Robert Izzard (AIfA, Bonn) Beer, Bureaucracy and Binary Stars 4 / 17

5 Night Sky Declination (Latitude) Yale Bright Star Catalogue, Stars Brighter than 5th Mag Right Ascension (Longitude) Robert Izzard (AIfA, Bonn) Beer, Bureaucracy and Binary Stars 5 / 17

6 Night Sky Binaries: 5%! Declination (Latitude) Yale Bright Star Catalogue, Stars Brighter than 5th Mag Right Ascension (Longitude) Robert Izzard (AIfA, Bonn) Beer, Bureaucracy and Binary Stars 6 / 17

7 Old stars are big: interaction Robert Izzard (AIfA, Bonn) Beer, Bureaucracy and Binary Stars 7 / 17

8 Old stars make heavy metal(s) M, Z = Z /5 Radius / R Time / Myr Robert Izzard (AIfA, Bonn) Beer, Bureaucracy and Binary Stars 8 / 17

9 Old stars make heavy metal(s) M, Z = Z /5 Radius / R Carbon Time / Myr Time / Myr Robert Izzard (AIfA, Bonn) Beer, Bureaucracy and Binary Stars 9 / 17

10 Old stars make heavy metal(s) M, Z = Z /5 Radius / R 6e e e e-7 1 Carbon Barium.5 2e e-7 Time / Myr Time / Myr Time / Myr Robert Izzard (AIfA, Bonn) Beer, Bureaucracy and Binary Stars 1 / 17

11 Old stars make heavy metal(s) M, Z = Z /5 Radius / R 6e e e e Carbon Barium Carbon.5 2e e-7 Time / Myr Time / Myr Time / Myr Radius / R Robert Izzard (AIfA, Bonn) Beer, Bureaucracy and Binary Stars 11 / 17

12 Big Science Problems Results of binary interaction models do not agree well with models! 1.8 Eccentricity log 1 (Period/days) This model is very approximate... can do better. Robert Izzard (AIfA, Bonn) Beer, Bureaucracy and Binary Stars 12 / 17

13 STAREVOL Stellar Evolution code Why Universite Libre de Bruxelles? Perfect code for late evolutionary phases Brussels binary observers group What is STAREVOL? Star = 1D, many shells Henyey/N-R solver Detailed single-star physics Truthfully, Why Brussels? Robert Izzard (AIfA, Bonn) Beer, Bureaucracy and Binary Stars 13 / 17

14 BINSTAR Based on STAREVOL Two stars Binary interactions Orbit Tides Mass/angular momentum transfer Simple OpenMP Graphical frontend Robert Izzard (AIfA, Bonn) Beer, Bureaucracy and Binary Stars 14 / 17

15 Where does the computational effort go? 13,,, years of binary star evolution: 1M + 1M wide binary, main sequence only Calculation Time Opacity 14% Nuclear rates 22% Nucleosynthesis 9% Eq. of State 22% Tides 6% Henyey <1%! Most of the time goes into computing (micro)physics shell by shell. Robert Izzard (AIfA, Bonn) Beer, Bureaucracy and Binary Stars 15 / 17

16 Shell-by-shell computation Most operations are shell by shell, could be massively parallel! Calculation Method Opacity Table lookup Nuclear rates Table lookup Nucleosynthesis Matrix calculations (*,+) Eq. of State Table and calculations Tides calculations Henyey Matrix calculations, serial Worth the GPU effort? Robert Izzard (AIfA, Bonn) Beer, Bureaucracy and Binary Stars 16 / 17

17 Future Prospects GPUs are an untapped resource which in stellar evolution studies Faster code: more stars Why? statistical studies stellar populations without previous approximations to compare with observations 1. statistically 2. quantitatively to constrain model parameters to understand the (astro)physics Tarantula Nebula, Large Magellanic Cloud Robert Izzard (AIfA, Bonn) Beer, Bureaucracy and Binary Stars 17 / 17

Robert Izzard Université Libre de Bruxelles

Robert Izzard Université Libre de Bruxelles Binary Star Populations: Keys to Understanding Stellar Astrophysics Robert Izzard Université Libre de Bruxelles with Onno Pols, Evert Glebbeek and Richard Stancliffe A Short Journey... Your Night Sky:

More information

Supernova Explosions. Novae

Supernova Explosions. Novae Supernova Explosions Novae Novae occur in close binary-star systems in which one member is a white dwarf. First, mass is transferred from the normal star to the surface of its white dwarf companion. 1

More information

Astronomy 102: Stars and Galaxies Examination 3 April 11, 2003

Astronomy 102: Stars and Galaxies Examination 3 April 11, 2003 Name: Seat Number: Astronomy 102: Stars and Galaxies Examination 3 April 11, 2003 Do not open the test until instructed to begin. Instructions: Write your answers in the space provided. If you need additional

More information

Understanding Black Hole

Understanding Black Hole Understanding Black Hole Formation and Natal Kicks: The Case of Cygnus X-1 TsingWai Wong Francesca Valsecchi, Tassos Fragos, Bart Willems, Vicky Kalogera Background & Purpose Find the mass relationship

More information

astronomy A planet was viewed from Earth for several hours. The diagrams below represent the appearance of the planet at four different times.

astronomy A planet was viewed from Earth for several hours. The diagrams below represent the appearance of the planet at four different times. astronomy 2008 1. A planet was viewed from Earth for several hours. The diagrams below represent the appearance of the planet at four different times. 5. If the distance between the Earth and the Sun were

More information

Evolution of Stars Population III: Population II: Population I:

Evolution of Stars Population III: Population II: Population I: Evolution of Stars 1. Formed from gas/dust cloud collapse from gravity 2. Fuse H to He on the Main Sequence. Then evolve off Main-sequence as they burn He and successive elements. 3. When nuclear fusion

More information

V. Astronomy Section

V. Astronomy Section EAS 100 Planet Earth Lecture Topics Brief Outlines V. Astronomy Section 1. Introduction, Astronomical Distances, Solar System Learning objectives: Develop an understanding of Earth s position in the solar

More information

Student Review Investigations in Earth and Space Science Semester A 2015 Examination

Student Review Investigations in Earth and Space Science Semester A 2015 Examination Investigations in Earth and Space Science Semester A Examination Test Description Length: 2 hours Items: 56 SR (85%), 2 BCRs (15%) Unit Approximate Number of Selected Response Items IESS Skills and Processes

More information

Chapter 15 The Milky Way Galaxy. The Milky Way

Chapter 15 The Milky Way Galaxy. The Milky Way Chapter 15 The Milky Way Galaxy The Milky Way Almost everything we see in the night sky belongs to the Milky Way We see most of the Milky Way as a faint band of light across the sky From the outside, our

More information

Supernova Explosions. Novae

Supernova Explosions. Novae Supernova Explosions Novae Novae occur in close binary-star systems in which one member is a white dwarf. First, mass is transferred from the normal star to the surface of its white dwarf companion. 1

More information

The Evolution of Low Mass Stars

The Evolution of Low Mass Stars The Evolution of Low Mass Stars Key Ideas: Low Mass = M < 4 M sun Stages of Evolution of a Low Mass star: Main Sequence star star star Asymptotic Giant Branch star Planetary Nebula phase White Dwarf star

More information

Curriculum vitae: Robert G. Izzard

Curriculum vitae: Robert G. Izzard Born 2nd November, 1976 British nationality ÞÞ Ö ØÖÓºÙÒ ¹ ÓÒÒº (personal) ÖÓ º ÞÞ Ö Ñ ÐºÓÑ Specialist areas of astrophysics Curriculum vitae: Robert G. Izzard W2 Professor of Astrophysics, Argelander-Institut

More information

STUDY GUIDE FOR PHYSICAL SCIENCE EXAM

STUDY GUIDE FOR PHYSICAL SCIENCE EXAM STUDY GUIDE FOR PHYSICAL SCIENCE EXAM 1 2017 VOCABULARY: Branches of science Density Low mass star High mass star Manipulated variable Responding variable Claim Inference Precision Density Accuracy Spectroscopy

More information

AST 101 Introduction to Astronomy: Stars & Galaxies

AST 101 Introduction to Astronomy: Stars & Galaxies AST 101 Introduction to Astronomy: Stars & Galaxies The H-R Diagram review So far: Stars on Main Sequence (MS) Next: - Pre MS (Star Birth) - Post MS: Giants, Super Giants, White dwarfs Star Birth We start

More information

Chapter 9: Measuring the Stars

Chapter 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 information

Lec 9: Stellar Evolution and DeathBirth and. Why do stars leave main sequence? What conditions are required for elements. Text

Lec 9: Stellar Evolution and DeathBirth and. Why do stars leave main sequence? What conditions are required for elements. Text 1 Astr 102 Lec 9: Stellar Evolution and DeathBirth and Evolution Why do stars leave main sequence? What conditions are required for elements Text besides Hydrogen to fuse, and why? How do stars die: white

More information

Lecture Tutorial: Using Astronomy Picture of the Day to learn about the life cycle of stars

Lecture Tutorial: Using Astronomy Picture of the Day to learn about the life cycle of stars Lecture Tutorial: Using Astronomy Picture of the Day to learn about the life cycle of stars For this exercise, you will need an ipad or computer and access to the internet. We will be using the website

More information

Galaxy classification

Galaxy classification Galaxy classification Questions of the Day What are elliptical, spiral, lenticular and dwarf galaxies? What is the Hubble sequence? What determines the colors of galaxies? Top View of the Milky Way The

More information

Lecture 1: Introduction. Literature: Onno Pols chapter 1, Prialnik chapter 1

Lecture 1: Introduction. Literature: Onno Pols chapter 1, Prialnik chapter 1 Lecture 1: Introduction Literature: Onno Pols chapter 1, Prialnik chapter 1!" Goals of the Course! Understand the global characteristics of stars! Relate relevant microphysics to the global stellar characteristics!

More information

The Deaths of Stars. The Southern Crab Nebula (He2-104), a planetary nebula (left), and the Crab Nebula (M1; right), a supernova remnant.

The Deaths of Stars. The Southern Crab Nebula (He2-104), a planetary nebula (left), and the Crab Nebula (M1; right), a supernova remnant. The Deaths of Stars The Southern Crab Nebula (He2-104), a planetary nebula (left), and the Crab Nebula (M1; right), a supernova remnant. Once the giant phase of a mediummass star ends, it exhales its outer

More information

8.8A describe components of the universe, including stars, nebulae, galaxies and use models such as HR diagrams for classification

8.8A describe components of the universe, including stars, nebulae, galaxies and use models such as HR diagrams for classification 8.8A describe components of the universe, including stars, nebulae, galaxies and use models such as HR diagrams for classification 8.8B recognize that the Sun is a medium-sized star near the edge of a

More information

10/26/ Star Birth. Chapter 13: Star Stuff. How do stars form? Star-Forming Clouds. Mass of a Star-Forming Cloud. Gravity Versus Pressure

10/26/ Star Birth. Chapter 13: Star Stuff. How do stars form? Star-Forming Clouds. Mass of a Star-Forming Cloud. Gravity Versus Pressure 10/26/16 Lecture Outline 13.1 Star Birth Chapter 13: Star Stuff How do stars form? Our goals for learning: How do stars form? How massive are newborn stars? Star-Forming Clouds Stars form in dark clouds

More information

The Stars. Chapter 14

The Stars. Chapter 14 The Stars Chapter 14 Great Idea: The Sun and other stars use nuclear fusion reactions to convert mass into energy. Eventually, when a star s nuclear fuel is depleted, the star must burn out. Chapter Outline

More information

CHARA/NPOI 2013 Science & Technology Review MIRC Observations of the O-star Triple Sigma Orionis

CHARA/NPOI 2013 Science & Technology Review MIRC Observations of the O-star Triple Sigma Orionis MIRC Observations of the O-star Triple Sigma Orionis Gail Schaefer Doug Gies John Monnier Nils Turner New Title: Do NPOI and CHARA Orbits Agree?... stay tuned... Sigma Orionis Image credit: Peter Wienerroither

More information

Stellar evolution Part I of III Star formation

Stellar evolution Part I of III Star formation Stellar evolution Part I of III Star formation The interstellar medium (ISM) The space between the stars is not completely empty, but filled with very dilute gas and dust, producing some of the most beautiful

More information

The light curves for a nova look like the following.

The light curves for a nova look like the following. End of high mass stars Nova Supernova Type I Type II Stellar nucleo-synthesis Stellar Recycling Nova (means new): is a star that suddenly increases greatly in brightness, then slowly fades back to its

More information

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?

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.

More information

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

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.

More information

Laboratory: Milky Way

Laboratory: Milky Way Department of Physics and Geology Laboratory: Milky Way Astronomy 1402 Equipment Needed Quantity Equipment Needed Quantity Milky Way galaxy Model 1 Ruler 1 1.1 Our Milky Way Part 1: Background Milky Way

More information

Astro 21 first lecture. stars are born but also helps us study how. Density increases in the center of the star. The core does change from hydrogen to

Astro 21 first lecture. stars are born but also helps us study how. Density increases in the center of the star. The core does change from hydrogen to Astro 21 first lecture The H-R H R Diagram helps us study how stars are born but also helps us study how they die. Stars spend most of their lives as main sequence stars. The core does change from hydrogen

More information

Life Cycle of a Star - Activities

Life Cycle of a Star - Activities Name: Class Period: Life Cycle of a Star - Activities A STAR IS BORN STAGES COMMON TO ALL STARS All stars start as a nebula. A nebula is a large cloud of gas and dust. Gravity can pull some of the gas

More information

Introduction to the Universe. What makes up the Universe?

Introduction 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

Ay 1 Lecture 2. Starting the Exploration

Ay 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 information

Phys 100 Astronomy (Dr. Ilias Fernini) Review Questions for Chapter 9

Phys 100 Astronomy (Dr. Ilias Fernini) Review Questions for Chapter 9 Phys 0 Astronomy (Dr. Ilias Fernini) Review Questions for Chapter 9 MULTIPLE CHOICE 1. We know that giant stars are larger in diameter than the sun because * a. they are more luminous but have about the

More information

Chapter 17 Lecture. The Cosmic Perspective Seventh Edition. Star Stuff Pearson Education, Inc.

Chapter 17 Lecture. The Cosmic Perspective Seventh Edition. Star Stuff Pearson Education, Inc. Chapter 17 Lecture The Cosmic Perspective Seventh Edition Star Stuff Star Stuff 17.1 Lives in the Balance Our goals for learning: How does a star's mass affect nuclear fusion? How does a star's mass affect

More information

FORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS

FORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS FORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS Main Categories of Compact Systems Formation of Compact Objects Mass and Angular Momentum Loss Evolutionary Links to Classes of Binary Systems Future Work

More information

ASTR 1P01 Test 1, September 2017 Page 1 BROCK UNIVERSITY

ASTR 1P01 Test 1, September 2017 Page 1 BROCK UNIVERSITY ASTR 1P01 Test 1, September 2017 Page 1 BROCK UNIVERSITY Test 1: Fall 2017 Number of pages: 10 Course: ASTR 1P01, Section 2 Number of students: 1300 Examination date: 30 September 2017 Time limit: 50 min

More information

Location, Location, Location Sailors relied on the astronomy (2000 B.C.) Universe ( ) Astronomy is the handmaiden to the sailor.

Location, Location, Location Sailors relied on the astronomy (2000 B.C.) Universe ( ) Astronomy is the handmaiden to the sailor. The Universe Chapter 1 Why was Astronomy important to the ancients? Natural Clocks Motion of the sun, moon, planets and stars plant crops, harvest crops Location, Location, Location Sailors relied on the

More information

Stellar mass black holes in young massive and open clusters and their role in gravitational-wave generation

Stellar mass black holes in young massive and open clusters and their role in gravitational-wave generation Stellar mass black holes in young massive and open clusters and their role in gravitational-wave generation Sambaran Banerjee Argelander-Institut für Astronomie (AIfA) and Helmholtz-Instituts für Strahlen-

More information

SUPPLEMENTARY INFORMATION

SUPPLEMENTARY INFORMATION 1. Identification of classical Cepheids: We identified three classical Cepheids amongst the 45 short-period variables discovered. Our sample includes classical Cepheids, type II Cepheids, eclipsing binaries

More information

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 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

More information

The Universe. is space and everything in it.

The Universe. is space and everything in it. The Universe is space and everything in it. Galaxies A galaxy is a supercluster of stars, gas, and dust that are held together by gravity. There are three main types of galaxies: Irregular Elliptical Spiral

More information

Spiral Density waves initiate star formation

Spiral Density waves initiate star formation Spiral Density waves initiate star formation A molecular cloud passing through the Sagittarius spiral arm Spiral arm Gas outflows from super supernova or O/B star winds Initiation of star formation Supernova

More information

ζ Pup: the merger of at least two massive stars?

ζ Pup: the merger of at least two massive stars? ζ Pup: the merger of at least two massive stars? Dany Vanbeveren Astrophysical Institute, Vrije Universiteit Brussel and Leuven Engineering College, GroupT, Association KU Leuven Abstract. We first discuss

More information

Nuclear Physics and Astrophysics of Exploding Stars

Nuclear Physics and Astrophysics of Exploding Stars Nuclear Physics and Astrophysics of Exploding Stars Lars Bildsten Kavli Institute for Theoretical Physics Department of Physics University of California, Santa Barbara Dan Kasen (UCSC), Kevin Moore (UCSB),

More information

Chapter 8: The Family of Stars

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

More information

2. Descriptive Astronomy ( Astronomy Without a Telescope )

2. Descriptive Astronomy ( Astronomy Without a Telescope ) How do we locate stars in the heavens? 2. Descriptive Astronomy ( Astronomy Without a Telescope ) What stars are visible from a given location? Where is the sun in the sky at any given time? Where are

More information

Photometric and spectroscopic observations of the outburst of the symbiotic star AG Draconis between March and June 2016

Photometric and spectroscopic observations of the outburst of the symbiotic star AG Draconis between March and June 2016 Photometric and spectroscopic observations of the outburst of the symbiotic star AG Draconis between March and June 2016 David Boyd Variable Star Section, British Astronomical Association, [davidboyd@orion.me.uk]

More information

Unit 7 Review Guide: The Universe

Unit 7 Review Guide: The Universe Unit 7 Review Guide: The Universe Light Year: Unit of distance used to measure the great vastness of space. Galaxy: Large group of stars, gas, and dust held together by gravity. Spiral Galaxy: Galaxy in

More information

Ch. 10: Star Formation of Planetary Systems. A summary of the process by which our solar system formed, according to the nebular theory.

Ch. 10: Star Formation of Planetary Systems. A summary of the process by which our solar system formed, according to the nebular theory. 1 Ch. 10: Star Formation of Planetary Systems A summary of the process by which our solar system formed, according to the nebular theory. Materials in the solar nebula. 2 3 Temperature differences in the

More information

Introduction to the Universe

Introduction to the Universe What makes up the Universe? Introduction to the Universe Book page 642-644 Objects in the Universe Astrophysics is the science that tries to make sense of the universe by - describing the Universe (Astronomy)

More information

The life of a low-mass star. Astronomy 111

The life of a low-mass star. Astronomy 111 Lecture 16: The life of a low-mass star Astronomy 111 Main sequence membership For a star to be located on the Main Sequence in the H-R diagram: must fuse Hydrogen into Helium in its core. must be in a

More information

Stars and Galaxies 1

Stars and Galaxies 1 Stars and Galaxies 1 Characteristics of Stars 2 Star - body of gases that gives off great amounts of radiant energy as light and heat 3 Most stars look white but are actually different colors Antares -

More information

Chapter 19: The Evolution of Stars

Chapter 19: The Evolution of Stars Chapter 19: The Evolution of Stars Why do stars evolve? (change from one state to another) Energy Generation fusion requires fuel, fuel is depleted [fig 19.2] at higher temperatures, other nuclear process

More information

GALAXIES AND STARS. 2. Which star has a higher luminosity and a lower temperature than the Sun? A Rigel B Barnard s Star C Alpha Centauri D Aldebaran

GALAXIES AND STARS. 2. Which star has a higher luminosity and a lower temperature than the Sun? A Rigel B Barnard s Star C Alpha Centauri D Aldebaran GALAXIES AND STARS 1. Compared with our Sun, the star Betelgeuse is A smaller, hotter, and less luminous B smaller, cooler, and more luminous C larger, hotter, and less luminous D larger, cooler, and more

More information

Starlight in the Night: Discovering the secret lives of stars

Starlight in the Night: Discovering the secret lives of stars Utah State University DigitalCommons@USU Public Talks Astrophysics 8-2-2008 Starlight in the Night: Discovering the secret lives of stars Shane L. Larson Utah State University Follow this and additional

More information

30 Doradus: Birthplace of giants and dwarfs

30 Doradus: Birthplace of giants and dwarfs Hubble Science Briefing 30 Doradus: Birthplace of giants and dwarfs Elena Sabbi June 7, 2012 Outline 1. How stars form and evolve; 2. How we can use star clusters to better understand high redshift galaxies;

More information

Geometry of Earth Sun System

Geometry of Earth Sun System 12S56 Geometry of Earth Sun System Figure below shows the basic geometry Northern Hemisphere Winter ω equator Earth s Orbit Ecliptic ω ω SUN equator Northern Hemisphere Spring Northern Hemisphere Fall

More information

Paul Broberg Ast 4001 Dec. 10, 2007

Paul Broberg Ast 4001 Dec. 10, 2007 Paul Broberg Ast 4001 Dec. 10, 2007 What are W-R stars? How do we characterize them? What is the life of these stars like? Early stages Evolution Death What can we learn from them? Spectra Dust 1867: Charles

More information

Late stages of stellar evolution for high-mass stars

Late stages of stellar evolution for high-mass stars Late stages of stellar evolution for high-mass stars Low-mass stars lead a relatively peaceful life in their old age: although some may gently blow off their outer envelopes to form beautiful planetary

More information

Lecture Outlines. Chapter 20. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.

Lecture Outlines. Chapter 20. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc. Lecture Outlines Chapter 20 Astronomy Today 8th Edition Chaisson/McMillan Chapter 20 Stellar Evolution Units of Chapter 20 20.1 Leaving the Main Sequence 20.2 Evolution of a Sun-Like Star 20.3 The Death

More information

First: Some Physics. Tides on the Earth. Lecture 11: Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes A2020 Prof. Tom Megeath. 1.

First: Some Physics. Tides on the Earth. Lecture 11: Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes A2020 Prof. Tom Megeath. 1. Lecture 11: Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes A2020 Prof. Tom Megeath First: Some Physics 1. Tides 2. Degeneracy Pressure Concept 1: How does gravity cause tides? R F tides

More information

Astronomy 25. Astronomy 25. Anything back then that could not be seen clearly was called a nebulae. detect fuzzy light objects.

Astronomy 25. Astronomy 25. Anything back then that could not be seen clearly was called a nebulae. detect fuzzy light objects. Astronomy 25 Astronomy 25 Before the 1920 s s telescopes would detect fuzzy light objects. Anything back then that could not be seen clearly was called a nebulae. Immanuel Kant (1724-1804) 1804) Kant had

More information

Lecture 24: Testing Stellar Evolution Readings: 20-6, 21-3, 21-4

Lecture 24: Testing Stellar Evolution Readings: 20-6, 21-3, 21-4 Lecture 24: Testing Stellar Evolution Readings: 20-6, 21-3, 21-4 Key Ideas HR Diagrams of Star Clusters Ages from the Main Sequence Turn-off Open Clusters Young clusters of ~1000 stars Blue Main-Sequence

More information

Chapter 14: The Bizarre Stellar Graveyard. Copyright 2010 Pearson Education, Inc.

Chapter 14: The Bizarre Stellar Graveyard. Copyright 2010 Pearson Education, Inc. Chapter 14: The Bizarre Stellar Graveyard Assignments 2 nd Mid-term to be held Friday Nov. 3 same basic format as MT1 40 mult. choice= 80 pts. 4 short answer = 20 pts. Sample problems on web page Origin

More information

Stellar Interior: Physical Processes

Stellar Interior: Physical Processes Physics Focus on Astrophysics Focus on Astrophysics Stellar Interior: Physical Processes D. Fluri, 29.01.2014 Content 1. Mechanical equilibrium: pressure gravity 2. Fusion: Main sequence stars: hydrogen

More information

Lecture 8. October 25, 2017 Lab 5

Lecture 8. October 25, 2017 Lab 5 Lecture 8 October 25, 2017 Lab 5 News Lab 2 & 3 Handed back next week (I hope). Lab 4 Due today Lab 5 (Transiting Exoplanets) Handed out and observing will start Friday. Due November 8 (or later) Stellar

More information

CONTENT EXPECTATIONS

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

More information

Astronomy 102: Stars and Galaxies Examination 3 Review Problems

Astronomy 102: Stars and Galaxies Examination 3 Review Problems Astronomy 102: Stars and Galaxies Examination 3 Review Problems Multiple Choice Questions: The first eight questions are multiple choice. Except where explicitly noted, only one answer is correct for each

More information

Review: HR Diagram. Label A, B, C respectively

Review: HR Diagram. Label A, B, C respectively Stellar Evolution Review: HR Diagram Label A, B, C respectively A C B a) A: White dwarfs, B: Giants, C: Main sequence b) A: Main sequence, B: Giants, C: White dwarfs c) A: Main sequence, B: White Dwarfs,

More information

Why Do Stars Leave the Main Sequence? Running out of fuel

Why Do Stars Leave the Main Sequence? Running out of fuel Star Deaths Why Do Stars Leave the Main Sequence? Running out of fuel Observing Stellar Evolution by studying Globular Cluster HR diagrams Plot stars in globular clusters in Hertzsprung-Russell diagram

More information

OPTION E, ASTROPHYSICS TEST REVIEW

OPTION E, ASTROPHYSICS TEST REVIEW IB PHYSICS Name: DEVIL PHYSICS Period: Date: BADDEST CLASS ON CAMPUS OPTION E, ASTROPHYSICS TEST REVIEW S1. This question is about the nature of certain stars on the Hertzsprung-Russell diagram and determining

More information

Astronomy 102: Stars and Galaxies Spring 2003 Final Exam Review Topics

Astronomy 102: Stars and Galaxies Spring 2003 Final Exam Review Topics Astronomy 102: Stars and Galaxies Spring 2003 Final Exam Review Topics The final exam will cover material from the whole course (including the galaxies and cosmology material from after Exam 3). The topics

More information

Chapter 17: Stellar Evolution

Chapter 17: Stellar Evolution Astr 2310 Thurs. Mar. 30, 2017 Today s Topics Chapter 17: Stellar Evolution Birth of Stars and Pre Main Sequence Evolution Evolution on and off the Main Sequence Solar Mass Stars Massive Stars Low Mass

More information

ASTR STELLAR PULSATION COMPONENT. Peter Wood Research School of Astronomy & Astrophysics

ASTR STELLAR PULSATION COMPONENT. Peter Wood Research School of Astronomy & Astrophysics ASTR 3007 - STELLAR PULSATION COMPONENT Peter Wood Research School of Astronomy & Astrophysics TOPICS COVERED Main types of variable stars Linear adiabatic pulsation theory => periods of pulsation Linear

More information

1. Star: A object made of gas found in outer space that radiates.

1. Star: A object made of gas found in outer space that radiates. 1. Star: A object made of gas found in outer space that radiates. 2. Stars produce extremely great quantities of energy through the process of. The chemical formula for nuclear fusion looks like this:

More information

Ay 20: Basic Astronomy and the Galaxy Fall Term Solution Set 4 Kunal Mooley (based on solutions by Swarnima Manohar, TA 2009)

Ay 20: Basic Astronomy and the Galaxy Fall Term Solution Set 4 Kunal Mooley (based on solutions by Swarnima Manohar, TA 2009) Ay 20: Basic Astronomy and the Galaxy Fall Term 2010 Solution Set 4 Kunal Mooley (based on solutions by Swarnima Manohar, TA 2009) Reporting an answer to unnecesary number of decimal places should be avoided.

More information

20. Stellar Death. Interior of Old Low-Mass AGB Stars

20. Stellar Death. Interior of Old Low-Mass AGB Stars 20. Stellar Death Low-mass stars undergo three red-giant stages Dredge-ups bring material to the surface Low -mass stars die gently as planetary nebulae Low -mass stars end up as white dwarfs High-mass

More information

10/17/2012. Stellar Evolution. Lecture 14. NGC 7635: The Bubble Nebula (APOD) Prelim Results. Mean = 75.7 Stdev = 14.7

10/17/2012. Stellar Evolution. Lecture 14. NGC 7635: The Bubble Nebula (APOD) Prelim Results. Mean = 75.7 Stdev = 14.7 1 6 11 16 21 26 31 36 41 46 51 56 61 66 71 76 81 86 91 96 10/17/2012 Stellar Evolution Lecture 14 NGC 7635: The Bubble Nebula (APOD) Prelim Results 9 8 7 6 5 4 3 2 1 0 Mean = 75.7 Stdev = 14.7 1 Energy

More information

Day, Night & the Seasons. Lecture 2 1/21/2014

Day, Night & the Seasons. Lecture 2 1/21/2014 Day, Night & the Seasons Lecture 2 1/21/2014 Logistics The following students see me after class: A. Gonzalez, Chen Anyone who was not here on first day see me after class Pin Numbers - if you have not

More information

PHYS 160 Astronomy Test #1 Fall 2017 Version B

PHYS 160 Astronomy Test #1 Fall 2017 Version B PHYS 160 Astronomy Test #1 Fall 2017 Version B 1 I. True/False (1 point each) Circle the T if the statement is true, or F if the statement is false on your answer sheet. 1. An object has the same weight,

More information

Beyond the Solar System 2006 Oct 17 Page 1 of 5

Beyond the Solar System 2006 Oct 17 Page 1 of 5 I. Stars have color, brightness, mass, temperature and size. II. Distances to stars are measured using stellar parallax a. The further away, the less offset b. Parallax angles are extremely small c. Measured

More information

Stellar Midlife. A. Main Sequence Lifetimes. (1b) Lifetime of Sun. Stellar Evolution Part II. A. Main Sequence Lifetimes. B. Giants and Supergiants

Stellar Midlife. A. Main Sequence Lifetimes. (1b) Lifetime of Sun. Stellar Evolution Part II. A. Main Sequence Lifetimes. B. Giants and Supergiants Stellar Evolution Part II 1 Stellar Midlife 2 Stellar Midlife A. Main Sequence Lifetimes B. Giants and Supergiants C. Variables (Cepheids) Dr. Bill Pezzaglia Updated Oct 9, 2006 A. Main Sequence Lifetimes

More information

Exam # 3 Tue 12/06/2011 Astronomy 100/190Y Exploring the Universe Fall 11 Instructor: Daniela Calzetti

Exam # 3 Tue 12/06/2011 Astronomy 100/190Y Exploring the Universe Fall 11 Instructor: Daniela Calzetti Exam # 3 Tue 12/06/2011 Astronomy 100/190Y Exploring the Universe Fall 11 Instructor: Daniela Calzetti INSTRUCTIONS: Please, use the `bubble sheet and a pencil # 2 to answer the exam questions, by marking

More information

Doppler Technique Measuring a star's Doppler shift can tell us its motion toward and away from us.

Doppler Technique Measuring a star's Doppler shift can tell us its motion toward and away from us. Doppler Technique Measuring a star's Doppler shift can tell us its motion toward and away from us. Current techniques can measure motions as small as 1 m/s (walking speed!). Sun motion due to: Jupiter:

More information

Dark Matter ASTR 2120 Sarazin. Bullet Cluster of Galaxies - Dark Matter Lab

Dark Matter ASTR 2120 Sarazin. Bullet Cluster of Galaxies - Dark Matter Lab Dark Matter ASTR 2120 Sarazin Bullet Cluster of Galaxies - Dark Matter Lab Mergers: Test of Dark Matter vs. Modified Gravity Gas behind DM Galaxies DM = location of gravity Gas = location of most baryons

More information

Astronomy 122 Midterm

Astronomy 122 Midterm Astronomy 122 Midterm This Class (Lecture 15): Stellar Evolution: The Main Sequence Next Class: Stellar Evolution: Post-Main Sequence Midterm on Thursday! Last week for Nightlabs 1 hour exam in this classroom

More information

Stellar Explosions (ch. 21)

Stellar Explosions (ch. 21) Stellar Explosions (ch. 21) First, a review of low-mass stellar evolution by means of an illustration I showed in class. You should be able to talk your way through this diagram and it should take at least

More information

Chapter 12 Stellar Evolution

Chapter 12 Stellar Evolution Chapter 12 Stellar Evolution Guidepost Stars form from the interstellar medium and reach stability fusing hydrogen in their cores. This chapter is about the long, stable middle age of stars on the main

More information

Stellar Death. Final Phases

Stellar Death. Final Phases Stellar Death Final Phases After the post-agb phase, the death of the star is close at hand. Function of Mass (For stars < ~ 4 solar masses) 1. Lowest mass stars will never have sufficient pressure and

More information

10-20 billion years old

10-20 billion years old Universe : 10-20 billion years old Big Bang Theory * the universe started at a single point * that point was extremely dense * it became unstable and expanded outward * The universe is still expanding

More information

What tool do astronomers use to understand the evolution of stars?

What tool do astronomers use to understand the evolution of stars? What tool do astronomers use to understand the evolution of stars? Groups indicate types of stars or stages in their evolution. What is plotted? How does an individual star move around the diagram? What

More information

Mass loss from stars

Mass loss from stars Mass loss from stars Can significantly affect a star s evolution, since the mass is such a critical parameter (e.g., L ~ M 4 ) Material ejected into interstellar medium (ISM) may be nuclear-processed:

More information

OPTION E, ASTROPHYSICS TEST REVIEW

OPTION E, ASTROPHYSICS TEST REVIEW IB PHYSICS Name: DEVIL PHYSICS Period: Date: # Marks: XX Raw Score: IB Curve: BADDEST CLASS ON CAMPUS OPTION E, ASTROPHYSICS TEST REVIEW S1. This question is about the nature of certain stars on the Hertzsprung-Russell

More information

Astronomy 103: First Exam

Astronomy 103: First Exam Name: Astronomy 103: First Exam Stephen Lepp September 21, 2010 Each question is worth 2 points. Write your name on this exam and on the scantron. Short Answer Mercury What is the closest Planet to the

More information

TA feedback forms are online!

TA feedback forms are online! 1 Announcements TA feedback forms are online! find the link at the class website. Please take 5 minutes to tell your TAs your opinion. In case you did not notice, the Final is set for 03/21 from 12:00-3:00

More information

THE 82ND ARTHUR H. COMPTON LECTURE SERIES

THE 82ND ARTHUR H. COMPTON LECTURE SERIES THE 82ND ARTHUR H. COMPTON LECTURE SERIES by Dr. Manos Chatzopoulos Enrico Fermi Postdoctoral Fellow FLASH Center for Computational Science Department of Astronomy & Astrophysics University of Chicago

More information

Evolution Beyond the Red Giants

Evolution Beyond the Red Giants Evolution Beyond the Red Giants Interior Changes Sub-giant star 1 Post-Helium Burning What happens when there is a new core of non-burning C and O? 1. The core must contract, which increases the pressure

More information

High Mass Stars and then Stellar Graveyard 7/16/09. Astronomy 101

High Mass Stars and then Stellar Graveyard 7/16/09. Astronomy 101 High Mass Stars and then Stellar Graveyard 7/16/09 Astronomy 101 Astronomy Picture of the Day Astronomy 101 Something Cool Betelgeuse Astronomy 101 Outline for Today Astronomy Picture of the Day Something

More information

High Mass Stars. Dr Ken Rice. Discovering Astronomy G

High Mass Stars. Dr Ken Rice. Discovering Astronomy G High Mass Stars Dr Ken Rice High mass star formation High mass star formation is controversial! May form in the same way as low-mass stars Gravitational collapse in molecular clouds. May form via competitive

More information