Planetary Nebulae evolve to White Dwarf Stars

Size: px
Start display at page:

Download "Planetary Nebulae evolve to White Dwarf Stars"

Transcription

1 Planetary Nebulae evolve to White Dwarf Stars

2 Planetary Nebulae When Red Giant exhausts its He fuel the C core contracts Low & medium-mass stars don t have enough gravitational energy to heat to core 6 x 10 8 K (needed to fuse Carbon) The He & H burning shells keep expanding star, till... outer envelope is gently blown away forms a planetary nebula Not directly related to actual planets (just looks like one) The remnant central star becomes a white dwarf

3 Planetary Nebulae Ring Nebula Hourglass Nebula The collapsing core becomes a White Dwarf

4 Planetary Nebulae Cat s Eye Nebula Twin Jet Nebula

5 Degenerate Core Leftover Central star of aplanetary Nebula heats up as it collapses. Star has insufficient mass to get hot enough to fuse Carbon. Gravity is finally stopped by the force of electron degeneracy pressure. The star is now stable...

6 Degeneracy Pressure Two particles cannot occupy the same space with the same momentum (energy). For very dense solids, the electrons cannot be in their ground states, they become very energetic---approaching the speed of light. the electrons play a game of musical chairs The pressure holding up the star no longer depends on temperature.

7 White Dwarfs... are stable: gravity vs. electron degeneracy pressure generate no new energy. slide down HR-diagram as they radiate their heat into space, getting cooler and fainter. are very dense; M packed into a sphere the size of the Earth!

8 White Dwarfs Degenerate matter obeys different laws of physics. The more mass the star has, the smaller the star becomes! increased gravity makes the star denser greater density increases degeneracy pressure to balance gravity

9 White Dwarfs Sirius B is the closest white dwarf to us Sirius A + B in X-rays

10 If WD in close binary: matter from giant star can "spill over" onto WD Pressure, temp on WD surface ingnite H fusion WD suddenly gets ,000 times brighter. White Dwarfs and Novae

11 Novae Though this shell contains a tiny amount of mass ( M ) it can cause the white dwarf to brighten by 10 magnitudes (10,000 times) in a few days.

12 Novae Because so little mass is lost during nova, explosion does not disrupt binary system. Ignition of infalling Hydrogen can recur again with periods ranging from months to thousands of years. the nova T Pyxidis viewed by Hubble Space Telescope

13 Limit on White Dwarf Mass Chandra formulated laws of degenerate matter. for this he won the Nobel Prize in Physics Predicted gravity will overcome pressure of electron degeneracy if white dwarf has mass > 1.4 M energetic electrons that cause this pressure reach speed of light Chandrasekhar Limit Subrahmanyan Chandrasekhar ( )

14 White Dwarf Supernovae If accretion brings mass of WD above Chandrasekhar limit, electron degeneracy can no longer support star. WD collapses Collapse raises core temperature and runaway carbon fusion begins, which ultimately leads to explosion of star. Such an exploding white dwarf is called a white dwarf supernova.

15 White Dwarf Supernovae Nova may reach absolute magnitude of 8 (ca. 100,000 Suns) White dwarf Supernova reach absolute mag of 19 (ca. 10 billion Suns). all reach nearly same peak luminosity (abs mag) white dwarf supernovae make good distance indicators More luminous than Cepheid variable stars so can be used to measure out to much greater distances than Cepheids There are two types of supernova: white dwarf: no prominent lines of hydrogen seen; white dwarfs thought to be origin. massive star: contains prominent hydrogen lines; results from explosion of single star.

16 Supernova Light Curves (Type II) (Type I)

17 Neutron Stars are the leftover cores from supernova explosions of massive stars If the core < 3 M, it will stop collapsing and be held up by neutron degeneracy pressure. Neutron stars are very dense (10 12 g/cm 3 ) 1.5 M with a diameter of 10 to 20 km They rotate very rapidly: Period = 0.03 to 4 sec Their magnetic fields are times stronger than Earth s. Chandra X-ray image of the neutron star left behind by a supernova observed in A.D The remnant is known as G

18 Pulsars In 1967, graduate student Jocelyn Bell and her advisor Anthony Hewish accidentally discovered a radio source in Vulpecula. Sharp pulse that recurred every 1.3 sec. They determined it was 300 pc away. They called it a pulsar, but what was it? Jocelyn Bell Light Curve of Jocelyn Bell s Pulsar

19 The mystery was solved when a pulsar was discovered in the heart of the Crab Nebula. The Crab pulsar also pulses in visual light.

20 Pulsars and Neutron Stars All pulsars are neutron stars, but all neutron stars are not pulsars!! Synchotron emission --- non-thermal process where light is emitted by charged particles moving close to the speed of light around magnetic fields. Emission (mostly radio) is concentrated at the magnetic poles and focused into a beam. Whether we see a pulsar depends on the geometry. if polar beam sweeps by Earth s direction once each rotation, the neutron star appears to be a pulsar if polar beam is always pointing toward or always pointing away from Earth, we do not see a pulsar

21 Pulsars and Neutron Stars Pulsars are the lighthouses of Galaxy!

22 Rotation Periods of Neutron Stars As a neutron star ages, it spins down. Youngest pulsars have shortest periods. Sometimes pulsar will suddenly speed up. This is called a glitch! There are some pulsars that have periods of several milliseconds. they tend to be in binaries.

23 Black Holes After a massive star goes supernova, if the core has a mass > 3 M, the force of gravity will be too strong for even neutron degeneracy to stop. Star will collapse into oblivion. GRAVITY FINALLY WINS!! Makes a black hole. Star becomes infinitely small creates a hole in spacetime >3 M compressed into tiny space => gravity HUGE! Newton s Law of Gravity breaks down

24 Schwarzschild Radius Radius at which escape speed = speed of light c = V esc = Sqrt[2 GM/R BH ] R BH = 2 GM/c 2 = 3 km (M/M sun ) Nothing (even light)can escape from inside R BH!!

25 Black Holes According to Einstein s Theory of Relativity, gravity is really the warping of spacetime about an object with mass. This means that even light is affected by gravity.

26 Warping of Space by Gravity Gravity curves space. bends light (even though it has no rest mass) within event horizon, it can not escape As matter approaches event horizon tidal forces become tremendous any objects would be streched like spaghetti

27 Warping of Time by Gravity In vicinity of black hole, even time slows down. If we launched a probe to it, as it approached the event horizon: e.g., it takes 50 min of time on mother ship for 15 min to elapse on probe from mother ship s view, probe takes forever to reach event horizon light from the probe is red-shifted probe would eventually disappear as light from it is red-shifted beyond radio From the probe s view: it heads straight into black hole light from the mother ship is blue-shifted

28 Summary on Stellar remnants M init < 8 M sun => Planetary nebula + white dwarf with M WD < 1. 4M sun R WD ~ R earth M init > 8 M sun => massive-star Supernova leaving behind either neutron star with: 1. 4 M sun < M NS < 3 M sun R NS ~ 15 km or a black hole with: M BH > 3 M sun R BH = 3 km (M/M sun )

Agenda. Degenerate Objects. 18. The Bizarre Stellar Graveyard. Degeneracy Pressure A Star s Final Battle. Our goals for learning:

Agenda. Degenerate Objects. 18. The Bizarre Stellar Graveyard. Degeneracy Pressure A Star s Final Battle. Our goals for learning: 18. The Bizarre Stellar Graveyard Now, my suspicion is that the Universe is not only queerer than we suppose, but queerer than we can suppose. Agenda Announce: Extra Credit presentations on April 18 H-R

More information

Ch. 16 & 17: Stellar Evolution and Death

Ch. 16 & 17: Stellar Evolution and Death Ch. 16 & 17: Stellar Evolution and Death Stars have lives: born, evolve, die Mass determines stellar evolution: Really Low Mass (0.08 to 0.4 M sun ) Low Mass: (0.4 to 4 M sun ) Long lives High Mass (4

More information

The Stellar Graveyard Neutron Stars & White Dwarfs

The Stellar Graveyard Neutron Stars & White Dwarfs The Stellar Graveyard Neutron Stars & White Dwarfs White Dwarfs White dwarfs are the remaining cores of low-mass (M < 8M sun ) stars Electron degeneracy pressure supports them against gravity Density ~

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

Chapter 18 The Bizarre Stellar Graveyard

Chapter 18 The Bizarre Stellar Graveyard Chapter 18 The Bizarre Stellar Graveyard 18.1 White Dwarfs Our goals for learning What is a white dwarf? What can happen to a white dwarf in a close binary system? What is a white dwarf? White Dwarfs White

More information

Stellar Evolution - Chapter 12 and 13. The Lives and Deaths of Stars White dwarfs, neutron stars and black holes

Stellar Evolution - Chapter 12 and 13. The Lives and Deaths of Stars White dwarfs, neutron stars and black holes Stellar Evolution - Chapter 12 and 13 The Lives and Deaths of Stars White dwarfs, neutron stars and black holes During the early stages of a star formation the objects are called a protostars. The internal

More information

The Bizarre Stellar Graveyard

The Bizarre Stellar Graveyard The Bizarre Stellar Graveyard 18.1 White Dwarfs Our goals for learning: What is a white dwarf? What can happen to a white dwarf in a close binary system? What is a white dwarf? White Dwarfs White dwarfs

More information

Protostars on the HR Diagram. Lifetimes of Stars. Lifetimes of Stars: Example. Pressure-Temperature Thermostat. Hydrostatic Equilibrium

Protostars on the HR Diagram. Lifetimes of Stars. Lifetimes of Stars: Example. Pressure-Temperature Thermostat. Hydrostatic Equilibrium Protostars on the HR Diagram Once a protostar is hot enough to start, it can blow away the surrounding gas Then it is visible: crosses the on the HR diagram The more the cloud, the it will form stars Lifetimes

More information

Chapter 14: The Bizarre Stellar Graveyard

Chapter 14: The Bizarre Stellar Graveyard Lecture Outline Chapter 14: The Bizarre Stellar Graveyard 14.1 White Dwarfs Our goals for learning: What is a white dwarf? What can happen to a white dwarf in a close binary system? What is a white dwarf?

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

Chapter 13: The Stellar Graveyard

Chapter 13: The Stellar Graveyard Chapter 13: The Stellar Graveyard Habbal Astro110 http://chandra.harvard.edu/photo/2001/1227/index.html Chapter 13 Lecture 26 1 Low mass star High mass (>8 M sun ) star Ends as a white dwarf. Ends in a

More information

Chapter 18 The Bizarre Stellar Graveyard. White Dwarfs. What is a white dwarf? Size of a White Dwarf White Dwarfs

Chapter 18 The Bizarre Stellar Graveyard. White Dwarfs. What is a white dwarf? Size of a White Dwarf White Dwarfs Chapter 18 The Bizarre Stellar Graveyard 18.1 White Dwarfs Our goals for learning What is a white dwarf? What can happen to a white dwarf in a close binary system? What is a white dwarf? White Dwarfs White

More information

Stellar remnants II. Neutron Stars 10/18/2010. (progenitor star 1.4 < M< 3 Msun) Stars, Galaxies & the Universe Announcements

Stellar remnants II. Neutron Stars 10/18/2010. (progenitor star 1.4 < M< 3 Msun) Stars, Galaxies & the Universe Announcements Stars, Galaxies & the Universe Announcements Exam #2 on Wednesday Review sheet and study guide posted by Thursday Use office hours and Astronomy Tutorial hours Covers material since Exam #1 (plus background

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

The Stellar Graveyard

The Stellar Graveyard Life and Death of High Mass Stars (M > 8 M sun ) AST 101 Introduction to Astronomy: Stars & Galaxies Last stage: Iron core surrounded by shells of increasingly lighter elements. Announcements MIDTERM #2

More information

11/1/16. Important Stuff (Section 001: 9:45 am) Important Stuff (Section 002, 1:00 pm) 14.1 White Dwarfs. Chapter 14: The Bizarre Stellar Graveyard

11/1/16. Important Stuff (Section 001: 9:45 am) Important Stuff (Section 002, 1:00 pm) 14.1 White Dwarfs. Chapter 14: The Bizarre Stellar Graveyard Important Stuff (Section 001: 9:45 am) The Second Midterm is Thursday, November 10 The Second Midterm will be given in a different room: Willey 175 Bring 2 pencils and a photo-id. In accordance with the

More information

Low mass stars. Sequence Star Giant. Red. Planetary Nebula. White Dwarf. Interstellar Cloud. White Dwarf. Interstellar Cloud. Planetary Nebula.

Low mass stars. Sequence Star Giant. Red. Planetary Nebula. White Dwarf. Interstellar Cloud. White Dwarf. Interstellar Cloud. Planetary Nebula. Low mass stars Interstellar Cloud Main Sequence Star Red Giant Planetary Nebula White Dwarf Interstellar Cloud Main Sequence Star Red Giant Planetary Nebula White Dwarf Low mass stars Interstellar Cloud

More information

11/1/17. Important Stuff (Section 001: 9:45 am) Important Stuff (Section 002, 1:00 pm) 14.1 White Dwarfs. Chapter 14: The Bizarre Stellar Graveyard

11/1/17. Important Stuff (Section 001: 9:45 am) Important Stuff (Section 002, 1:00 pm) 14.1 White Dwarfs. Chapter 14: The Bizarre Stellar Graveyard 11/1/17 Important Stuff (Section 001: 9:45 am) The Second Midterm is Thursday, November 9 The Second Midterm will be given in a different room: Willey 175 Bring 2 pencils and a photo-id. In accordance

More information

Astro 1050 Fri. Apr. 10, 2015

Astro 1050 Fri. Apr. 10, 2015 Astro 1050 Fri. Apr. 10, 2015 Today: Continue Ch. 13: Star Stuff Reading in Bennett: For Monday: Finish Chapter 13 Star Stuff Reminders: Ch. 12 HW now on Mastering Astronomy, due Monday. Ch. 13 will be

More information

Chapter 18 Lecture. The Cosmic Perspective Seventh Edition. The Bizarre Stellar Graveyard Pearson Education, Inc.

Chapter 18 Lecture. The Cosmic Perspective Seventh Edition. The Bizarre Stellar Graveyard Pearson Education, Inc. Chapter 18 Lecture The Cosmic Perspective Seventh Edition The Bizarre Stellar Graveyard The Bizarre Stellar Graveyard 18.1 White Dwarfs Our goals for learning: What is a white dwarf? What can happen to

More information

The Death of Stars. Today s Lecture: Post main-sequence (Chapter 13, pages ) How stars explode: supernovae! White dwarfs Neutron stars

The Death of Stars. Today s Lecture: Post main-sequence (Chapter 13, pages ) How stars explode: supernovae! White dwarfs Neutron stars The Death of Stars Today s Lecture: Post main-sequence (Chapter 13, pages 296-323) How stars explode: supernovae! White dwarfs Neutron stars White dwarfs Roughly the size of the Earth with the mass of

More information

A100 Exploring the Universe: Stellar Remnants. Martin D. Weinberg UMass Astronomy

A100 Exploring the Universe: Stellar Remnants. Martin D. Weinberg UMass Astronomy A100 Exploring the Universe: Stellar Remnants Martin D. Weinberg UMass Astronomy astron100-mdw@courses.umass.edu October 28, 2014 Read: S3, Chap 18 10/28/14 slide 1 Exam #2: November 04 One week from today!

More information

A100 Exploring the Universe: Stellar Remnants. Martin D. Weinberg UMass Astronomy

A100 Exploring the Universe: Stellar Remnants. Martin D. Weinberg UMass Astronomy A100 Exploring the Universe: Stellar Remnants Martin D. Weinberg UMass Astronomy astron100-mdw@courses.umass.edu March 24, 2015 Read: S3, Chap 18 03/24/15 slide 1 Exam #2: March 31 One week from today!

More information

White dwarfs are the remaining cores of dead stars. Electron degeneracy pressure supports them against the crush of gravity. The White Dwarf Limit

White dwarfs are the remaining cores of dead stars. Electron degeneracy pressure supports them against the crush of gravity. The White Dwarf Limit The Bizarre Stellar Graveyard Chapter 18 Lecture The Cosmic Perspective 18.1 White Dwarfs Our goals for learning: What is a white dwarf? What can happen to a white dwarf in a close binary system? Seventh

More information

Chapter 13 Notes The Deaths of Stars Astronomy Name: Date:

Chapter 13 Notes The Deaths of Stars Astronomy Name: Date: Chapter 13 Notes The Deaths of Stars Astronomy Name: Date: I. The End of a Star s Life When all the fuel in a star is used up, will win over pressure and the star will die nuclear fuel; gravity High-mass

More information

Neutron Stars. Chapter 14: Neutron Stars and Black Holes. Neutron Stars. What s holding it up? The Lighthouse Model of Pulsars

Neutron Stars. Chapter 14: Neutron Stars and Black Holes. Neutron Stars. What s holding it up? The Lighthouse Model of Pulsars Neutron Stars Form from a 8-20 M Sun star Chapter 14: Neutron Stars and Black Holes Leftover 1.4-3 M Sun core after supernova Neutron Stars consist entirely of neutrons (no protons) Neutron Star (tennis

More information

Evolution of High Mass stars

Evolution of High Mass stars Evolution of High Mass stars Neutron Stars A supernova explosion of a M > 8 M Sun star blows away its outer layers. The central core will collapse into a compact object of ~ a few M Sun. Pressure becomes

More information

Gravity simplest. fusion

Gravity simplest. fusion Gravity simplest fusion The life of a star has a complex relationship with gravity: 1. Gravity is what brings the original dust together to make a star 2. Gravity wants to crush the star Gravity pulls

More information

21. Neutron Stars. The Crab Pulsar: On & Off. Intensity Variations of a Pulsar

21. Neutron Stars. The Crab Pulsar: On & Off. Intensity Variations of a Pulsar 21. Neutron Stars Neutron stars were proposed in the 1930 s Pulsars were discovered in the 1960 s Pulsars are rapidly rotating neutron stars Pulsars slow down as they age Neutron stars are superfluid &

More information

Special Relativity. Principles of Special Relativity: 1. The laws of physics are the same for all inertial observers.

Special Relativity. Principles of Special Relativity: 1. The laws of physics are the same for all inertial observers. Black Holes Special Relativity Principles of Special Relativity: 1. The laws of physics are the same for all inertial observers. 2. The speed of light is the same for all inertial observers regardless

More information

H-R Diagram. Outline - March 25, Build-up of Inert Helium Core. Evolution of a Low-Mass Star

H-R Diagram. Outline - March 25, Build-up of Inert Helium Core. Evolution of a Low-Mass Star Outline - March 25, 2010 H-R Diagram Recap: Evolution and death of low mass stars (pgs. 566-572) About 90% of stars in the sky are Main Sequence stars Evolution and death of high mass stars (pgs. 572-581)

More information

Stars with Mⵙ go through two Red Giant Stages

Stars with Mⵙ go through two Red Giant Stages Astronomy A. Dayle Hancock adhancock@wm.edu Small 239 Office hours: MTWR 10-11am Death of Stars Nuclear reactions in small stars How stars disperse carbon How low mass stars die The nature of white dwarfs

More information

Astronomy Ch. 22 Neutron Stars and Black Holes. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.

Astronomy Ch. 22 Neutron Stars and Black Holes. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. Name: Period: Date: Astronomy Ch. 22 Neutron Stars and Black Holes MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) In a neutron star, the core

More information

Chapter 13 2/19/2014. Lecture Outline Neutron Stars. Neutron Stars and Black Holes Neutron Stars. Units of Chapter

Chapter 13 2/19/2014. Lecture Outline Neutron Stars. Neutron Stars and Black Holes Neutron Stars. Units of Chapter 13.1 Neutron Stars Lecture Outline Chapter 13 Neutron Stars and After a Type I supernova, little or nothing remains of the original star. After a Type II supernova, part of the core may survive. It is

More information

Stellar Remnants. White Dwarfs Neutron Stars Black Holes

Stellar Remnants. White Dwarfs Neutron Stars Black Holes Stellar Remnants White Dwarfs Neutron Stars Black Holes 1 Announcements q Homework # 5 is due today. q Homework # 6 starts today, Nov 15th. Due on Tuesday, Nov 22nd. 2 Assigned Reading Chapters: 64.4,

More information

BANG! Structure of a White Dwarf NO energy production gravity = degenerate gas pressure as it cools, becomes Black Dwarf. Lives of High Mass Stars

BANG! Structure of a White Dwarf NO energy production gravity = degenerate gas pressure as it cools, becomes Black Dwarf. Lives of High Mass Stars Structure of a White Dwarf NO energy production gravity = degenerate gas pressure as it cools, becomes Black Dwarf Mass Limit for White Dwarfs S. Chandrasekhar (1983 Nobel Prize) -calculated max. mass

More information

Astronomy Notes Chapter 13.notebook. April 11, 2014

Astronomy Notes Chapter 13.notebook. April 11, 2014 All stars begin life in a similar way the only difference is in the rate at which they move through the various stages (depends on the star's mass). A star's fate also depends on its mass: 1) Low Mass

More information

Neutron Stars. are as small as a city (~10 km) But as massive as the Sun!

Neutron Stars. are as small as a city (~10 km) But as massive as the Sun! Neutron Stars are as small as a city (~10 km) But as massive as the Sun! Extra-Terrestrial Mystery...! In 1967, graduate student Jocelyn Bell helped build a radio telescope in England.! She found a source

More information

Astronomy 110: SURVEY OF ASTRONOMY. 11. Dead Stars. 1. White Dwarfs and Supernovae. 2. Neutron Stars & Black Holes

Astronomy 110: SURVEY OF ASTRONOMY. 11. Dead Stars. 1. White Dwarfs and Supernovae. 2. Neutron Stars & Black Holes Astronomy 110: SURVEY OF ASTRONOMY 11. Dead Stars 1. White Dwarfs and Supernovae 2. Neutron Stars & Black Holes Low-mass stars fight gravity to a standstill by becoming white dwarfs degenerate spheres

More information

Death of stars is based on. one thing mass.

Death of stars is based on. one thing mass. Death of stars is based on one thing mass. Not the mass they have when born, but the mass they have when they die. Star Death for mass 1.4 solar masses and less. These stars started big 7.5-10 solar masses.

More information

Life and Evolution of a Massive Star. M ~ 25 M Sun

Life and Evolution of a Massive Star. M ~ 25 M Sun Life and Evolution of a Massive Star M ~ 25 M Sun Birth in a Giant Molecular Cloud Main Sequence Post-Main Sequence Death The Main Sequence Stars burn H in their cores via the CNO cycle About 90% of a

More information

Astronomy 113. Dr. Joseph E. Pesce, Ph.D. Dr. Joseph E. Pesce, Ph.D.

Astronomy 113. Dr. Joseph E. Pesce, Ph.D. Dr. Joseph E. Pesce, Ph.D. Astronomy 113 Dr. Joseph E. Pesce, Ph.D. Stellar Deaths/Endpoints 13-2 Low Mass Stars ³ Like the Sun (< 2 M ) ² Live about 10 billion years (sun is middle aged) ² Create elements through Carbon, Nitrogen,

More information

Fate of Stars. relative to Sun s mass

Fate of Stars. relative to Sun s mass INITIAL MASS relative to Sun s mass M < 0.01 Fate of Stars Final State planet.01 < M

More information

The Death of Stars. White Dwarfs, Neutron Stars and Black Holes. White Dwarfs

The Death of Stars. White Dwarfs, Neutron Stars and Black Holes. White Dwarfs The Death of Stars White Dwarfs, Neutron Stars and Black Holes White Dwarfs Formed when stars like our Sun reach the end of their life When the Sun s fuel is spent, it will collapse. Don t worry, that

More information

Lecture Outlines. Chapter 22. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc.

Lecture Outlines. Chapter 22. Astronomy Today 8th Edition Chaisson/McMillan Pearson Education, Inc. Lecture Outlines Chapter 22 Astronomy Today 8th Edition Chaisson/McMillan Chapter 22 Neutron Stars and Black Holes Units of Chapter 22 22.1 Neutron Stars 22.2 Pulsars 22.3 Neutron-Star Binaries 22.4 Gamma-Ray

More information

CHAPTER 14 II Stellar Evolution

CHAPTER 14 II Stellar Evolution 14-5. Supernova CHAPTER 14 II Stellar Evolution Exactly which stars become supernovae is not yet clear, but more than likely they are massive stars that become highly evolved. A star that develops an iron

More information

Neutron Stars. We now know that SN 1054 was a Type II supernova that ended the life of a massive star and left behind a neutron star.

Neutron Stars. We now know that SN 1054 was a Type II supernova that ended the life of a massive star and left behind a neutron star. Neutron Stars Neutron Stars The emission from the supernova that produced the crab nebula was observed in 1054 AD by Chinese, Japanese, Native Americans, and Persian/Arab astronomers as being bright enough

More information

Nuclear Synthesis. PHYS 162 Lectures 10a,b 1

Nuclear Synthesis. PHYS 162 Lectures 10a,b 1 Nuclear Synthesis All elements heavier than Helium are made inside stars up to Iron - fusion in Red Giants heavier than Iron (and some lighter) - Supernova explosions Stars lose matter at end of life-cycle

More information

Astronomy 104: Stellar Astronomy

Astronomy 104: Stellar Astronomy Astronomy 104: Stellar Astronomy Lecture 19: Stellar Remnants (Hanging Out with the Degenerates) Spring Semester 2013 Dr. Matt Craig 1 1 Things To Do Today and Next Time Chapter 12.2 (Neutron Stars) Chapter

More information

Chapter 14. Outline. Neutron Stars and Black Holes. Note that the following lectures include. animations and PowerPoint effects such as

Chapter 14. Outline. Neutron Stars and Black Holes. Note that the following lectures include. animations and PowerPoint effects such as 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 14 Neutron

More information

What is a star? A body of gases that gives off tremendous amounts of energy in the form of light & heat. What star is closest to the earth?

What is a star? A body of gases that gives off tremendous amounts of energy in the form of light & heat. What star is closest to the earth? Stars What is a star? A body of gases that gives off tremendous amounts of energy in the form of light & heat. What star is closest to the earth? Answer: The SUN It s about 150,000,000 km from earth =

More information

measured to be 10,000K, its small mass and faint luminosity did not make sense in the context of the mass-luminosity relation for stars.

measured to be 10,000K, its small mass and faint luminosity did not make sense in the context of the mass-luminosity relation for stars. 8.4 White Dwarfs As an asymptotic giant branch star becomes larger and more luminous, the rate at which is loses mass also increases. For stars less than 8 solar masses, a strong stellar wind develops

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

Neutron Stars. Properties of Neutron Stars. Formation of Neutron Stars. Chapter 14. Neutron Stars and Black Holes. Topics for Today s Class

Neutron Stars. Properties of Neutron Stars. Formation of Neutron Stars. Chapter 14. Neutron Stars and Black Holes. Topics for Today s Class Foundations of Astronomy 13e Seeds Phys1403 Introductory Astronomy Instructor: Dr. Goderya Chapter 14 Neutron Stars and Black Holes Cengage Learning 2016 Topics for Today s Class Neutron Stars What is

More information

Beyond Our Solar System Chapter 24

Beyond Our Solar System Chapter 24 Beyond Our Solar System Chapter 24 PROPERTIES OF STARS Distance Measuring a star's distance can be very difficult Stellar parallax Used for measuring distance to a star Apparent shift in a star's position

More information

Comparing a Supergiant to the Sun

Comparing a Supergiant to the Sun The Lifetime of Stars Once a star has reached the main sequence stage of it life, it derives its energy from the fusion of hydrogen to helium Stars remain on the main sequence for a long time and most

More information

Stellar Astronomy Sample Questions for Exam 4

Stellar Astronomy Sample Questions for Exam 4 Stellar Astronomy Sample Questions for Exam 4 Chapter 15 1. Emission nebulas emit light because a) they absorb high energy radiation (mostly UV) from nearby bright hot stars and re-emit it in visible wavelengths.

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

Termination of Stars

Termination of Stars Termination of Stars Some Quantum Concepts Pauli Exclusion Principle: "Effectively limits the amount of certain kinds of stuff that can be crammed into a given space (particles with personal space ). When

More information

ASTR 200 : Lecture 20. Neutron stars

ASTR 200 : Lecture 20. Neutron stars ASTR 200 : Lecture 20 Neutron stars 1 Equation of state: Degenerate matter We saw that electrons exert a `quantum mechanical' pressure. This is because they are 'fermions' and are not allowed to occupy

More information

ASTR Midterm 2 Phil Armitage, Bruce Ferguson

ASTR Midterm 2 Phil Armitage, Bruce Ferguson ASTR 1120-001 Midterm 2 Phil Armitage, Bruce Ferguson SECOND MID-TERM EXAM MARCH 21 st 2006: Closed books and notes, 1 hour. Please PRINT your name and student ID on the places provided on the scan sheet.

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

Chapter 18 Reading Quiz Clickers. The Cosmic Perspective Seventh Edition. The Bizarre Stellar Graveyard Pearson Education, Inc.

Chapter 18 Reading Quiz Clickers. The Cosmic Perspective Seventh Edition. The Bizarre Stellar Graveyard Pearson Education, Inc. Reading Quiz Clickers The Cosmic Perspective Seventh Edition The Bizarre Stellar Graveyard 18.1 White Dwarfs What is a white dwarf? What can happen to a white dwarf in a close binary system? What supports

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

Assignment 9. Multiple Choice Identify the letter of the choice that best completes the statement or answers the question.

Assignment 9. Multiple Choice Identify the letter of the choice that best completes the statement or answers the question. Assignment 9 Multiple Choice Identify the letter of the choice that best completes the statement or answers the question. 1. The astrophysicist who first calculated the highest mass that a dying star can

More information

Neutron Stars, Pulsars, Magnetars, and Black Holes the corpses of high-mass stars

Neutron Stars, Pulsars, Magnetars, and Black Holes the corpses of high-mass stars Neutron Stars, Pulsars, Magnetars, and Black Holes the corpses of high-mass stars Combination X-ray & visible light image of the Crab Nebula Pulsar From Chandra X-ray Observatory and Hubble Space Telescope

More information

Pulsars - a new tool for astronomy and physics

Pulsars - a new tool for astronomy and physics 1 Reading: Chapter 24, Sect. 24.5-24.6; Chap. 20, Chap. 25, Sec. 25.1 Exam 2: Thursday, March 22; essay question given on Tuesday, March 20 Last time:death of massive stars - supernovae & neutron stars

More information

Physics HW Set 3 Spring 2015

Physics HW Set 3 Spring 2015 1) If the Sun were replaced by a one solar mass black hole 1) A) life here would be unchanged. B) we would still orbit it in a period of one year. C) all terrestrial planets would fall in immediately.

More information

Explain how the sun converts matter into energy in its core. Describe the three layers of the sun s atmosphere.

Explain how the sun converts matter into energy in its core. Describe the three layers of the sun s atmosphere. Chapter 29 and 30 Explain how the sun converts matter into energy in its core. Describe the three layers of the sun s atmosphere. Explain how sunspots are related to powerful magnetic fields on the sun.

More information

Prentice Hall EARTH SCIENCE

Prentice Hall EARTH SCIENCE Prentice Hall EARTH SCIENCE Tarbuck Lutgens Chapter 25 Beyond Our Solar System 25.1 Properties of Stars Characteristics of Stars A constellation is an apparent group of stars originally named for mythical

More information

Fate of Stars. INITIAL MASS Final State relative to Sun s mass

Fate of Stars. INITIAL MASS Final State relative to Sun s mass Fate of Stars INITIAL MASS Final State relative to Sun s mass M < 0.01 planet.01 < M

More information

This class: Life cycle of high mass stars Supernovae Neutron stars, pulsars, pulsar wind nebulae, magnetars Quark-nova stars Gamma-ray bursts (GRBs)

This class: Life cycle of high mass stars Supernovae Neutron stars, pulsars, pulsar wind nebulae, magnetars Quark-nova stars Gamma-ray bursts (GRBs) This class: Life cycle of high mass stars Supernovae Neutron stars, pulsars, pulsar wind nebulae, magnetars Quark-nova stars Gamma-ray bursts (GRBs)!1 Cas$A$ All$Image$&$video$credits:$Chandra$X7ray$ Observatory$

More information

The Night Sky. The Universe. The Celestial Sphere. Stars. Chapter 14

The Night Sky. The Universe. The Celestial Sphere. Stars. Chapter 14 The Night Sky The Universe Chapter 14 Homework: All the multiple choice questions in Applying the Concepts and Group A questions in Parallel Exercises. Celestial observation dates to ancient civilizations

More information

Supernovae, Neutron Stars, Pulsars, and Black Holes

Supernovae, Neutron Stars, Pulsars, and Black Holes Supernovae, Neutron Stars, Pulsars, and Black Holes Massive stars and Type II supernovae Massive stars (greater than 8 solar masses) can create core temperatures high enough to burn carbon and heavier

More information

Astronomy. Chapter 15 Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes

Astronomy. Chapter 15 Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes Astronomy Chapter 15 Stellar Remnants: White Dwarfs, Neutron Stars, and Black Holes are hot, compact stars whose mass is comparable to the Sun's and size to the Earth's. A. White dwarfs B. Neutron stars

More information

Announcements. L! m 3.5 BRIGHT FAINT. Mass Luminosity Relation: Why? Homework#3 will be handed out at the end of this lecture.

Announcements. L! m 3.5 BRIGHT FAINT. Mass Luminosity Relation: Why? Homework#3 will be handed out at the end of this lecture. Announcements BRIGHT Homework#3 will be handed out at the end of this lecture. Due October 14 (next Thursday) Review of Mid-term exam will be handed out Tuesday. Mid-term exam will be variants (if not

More information

Star formation and Evolution

Star formation and Evolution Star formation and Evolution 1 Star formation and Evolution Stars burn fuel to produce energy and shine so they must evolve and live through a life cycle In the Milky Way we see stars at every stage of

More information

Lecture 23 Stellar Evolution & Death (High Mass) November 21, 2018

Lecture 23 Stellar Evolution & Death (High Mass) November 21, 2018 Lecture 23 Stellar Evolution & Death (High Mass) November 21, 2018 1 2 High Mass Stars (M > 5 M ) Section 13.3 Bennett, The Essential Cosmic Perspective, 7 th ed. High mass stars have: More mass Greater

More information

Hydrostatic Equilibrium in an ordinary star:

Hydrostatic Equilibrium in an ordinary star: Hydrostatic Equilibrium in an ordinary star: Pressure due to gravity is balanced by pressure of the ionized gas in the star which behaves like an ideal gas. Radiation leaving from the surface determines

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

READ: Chapter 11.1, 11.2 (11.2.1, only), 11.3(

READ: Chapter 11.1, 11.2 (11.2.1, only), 11.3( HW READ: Chapter 11.1, 11.2 (11.2.1,11.2.2 only), 11.3( 11.3.1,11.3.2 only), 11.4,11.5 Question 11.2(HW#15) Problems 1(HW#16) (part a: recall: basic KE=1/2mv 2,Part tb: recall momentum conservation M f

More information

Objectives. HR Diagram

Objectives. HR Diagram Objectives HR Diagram Questions from Yesterday Centripetal Force perpendicular to the rotation axis Acts to slow down collapse Strongest 90 deg from rotation axis Particles with an angle < 90 feel the

More information

MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.

MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. HW3 Name MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) A surface explosion on a white dwarf, caused by falling matter from the atmosphere of

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

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 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?

More information

AST 101 Introduction to Astronomy: Stars & Galaxies

AST 101 Introduction to Astronomy: Stars & Galaxies AST 101 Introduction to Astronomy: Stars & Galaxies Life and Death of High Mass Stars (M > 8 M sun ) REVIEW Last stage: Iron core surrounded by shells of increasingly lighter elements. REVIEW When mass

More information

AST 301 Introduction to Astronomy

AST 301 Introduction to Astronomy AST 301 Introduction to Astronomy John Lacy RLM 16.332 471-1469 lacy@astro.as.utexas.edu Myoungwon Jeon RLM 16.216 471-0445 myjeon@astro.as.utexas.edu Bohua Li RLM 16.212 471-8443 bohuali@astro.as.utexas.edu

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

Properties of Stars. Characteristics of Stars

Properties of Stars. Characteristics of Stars Properties of Stars Characteristics of Stars A constellation is an apparent group of stars originally named for mythical characters. The sky contains 88 constellations. Star Color and Temperature Color

More information

Cassiopeia A: Supernova Remnant

Cassiopeia A: Supernova Remnant Crab Nebula: Pulsar During a supernova, the core of a massive star can be compressed to form a rapidly rotating ball composed mostly of neutrons that is only twelve miles in diameter. A teaspoon of such

More information

Death of Stars Part II Neutron Stars

Death of Stars Part II Neutron Stars Death of Stars Part II Neutron Stars 1 REMEMBER THIS!? 2 Guiding Questions 1. What led scientists to the idea of a neutron star? 2. What are pulsars, and how were they discovered? 3. How did astronomers

More information

Today. Logistics. Visible vs. X-ray X. Synchrotron Radiation. Pulsars and Neutron Stars. ASTR 1040 Accel Astro: Stars & Galaxies

Today. Logistics. Visible vs. X-ray X. Synchrotron Radiation. Pulsars and Neutron Stars. ASTR 1040 Accel Astro: Stars & Galaxies ASTR 1040 Accel Astro: Stars & Galaxies Today Binary mass transfer Joys of nearest supernova: SN 1987A How mass transfer from binary companion can spin-up pulsar White dwarf supernovae from mass transfer

More information

Neutron Stars, Black Holes, Pulsars and More

Neutron Stars, Black Holes, Pulsars and More Neutron Stars, Black Holes, Pulsars and More October 30, 2002 1) Star Clusters 2) Type II Supernova 3) Neutron Stars 4) Black Holes 5) More Gravity Announcements Extra Credit there is an extra credit assignment

More information

1 The Life Cycle of a Star

1 The Life Cycle of a Star CHAPTER 1 The Life Cycle of a Star Describe the life cycle of various size stars. Rings of glowing gas encircling Supernova 1987A, about 179,000 light-years away in the Large Magellanic Cloud, one of the

More information

Fate of Stars. relative to Sun s mass

Fate of Stars. relative to Sun s mass INITIAL MASS relative to Sun s mass M < 0.01 Fate of Stars Final State planet.01 < M

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

Dead & Variable Stars

Dead & Variable Stars Dead & Variable Stars Supernovae Death of massive Stars As the core collapses, it overshoots and bounces A shock wave travels through the star and blows off the outer layers, including the heavy elements

More information

Prof. Kenney Class 8 June 6, 2018

Prof. Kenney Class 8 June 6, 2018 Prof. Kenney Class 8 June 6, 2018 differences in textbook editions 10 th ed vs 8 th & 9 th ed all chapter assignments starting with ch 21 on are shifted by 1 in 10th edition relative to 8th, 9th editions

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

A Star Becomes a Star

A Star Becomes a Star A Star Becomes a Star October 28, 2002 1) Stellar lifetime 2) Red Giant 3) White Dwarf 4) Supernova 5) More massive stars Review Solar winds/sunspots Gases and Dust Molecular clouds Protostars/Birth of

More information