Relativity and Black Holes

Size: px
Start display at page:

Download "Relativity and Black Holes"

Transcription

1 Relativity and Black Holes Post-MS Evolution of Very High Mass (>15 M Θ ) Stars similar to high mass except more rapid lives end in Type II supernova explosions main difference: mass of iron core at end of fusion > 3 M Θ core is too massive to form a neutron star! must collapse into something even denser a black hole! Escape Velocity, v e Measure of gravitational strength Minimum speed to escape the gravity of an object e.g. Earth, v e = 11.2 km/s v e mass v e size v e highest for objects which are small and massive i.e. dense! Neutron Stars, v e = 0.5c A neutron star only has to become 25% smaller in order to make v e = c Such an object is so dense that not even light can escape! Such an object is called a black hole! Problem: if light has no mass, how can it be affected by gravity? Newton s Theory of gravity has no explanation for this! To understand the properties of black holes we need a new theory of gravity! Einstein s Relativity! 1

2 Relative Motion Since everything in the Universe is in motion, measurements can only be made relatively and not absolutely! The Principles of Relativity 1. The Laws of Physics are the same for everyone and are independent of our location or motion in the Universe 2. The speed of light, c is constant and is the same for everyone and independent of our location or motion in the Universe Everything else is relative! Person Running Towards a Ball Person Traveling Towards Photon A photon always travels towards an observer at the speed of light, c regardless of their motion! Special Theory of Relativity (1905) Only deals with motion in straight lines and at constant speeds Is not a theory of gravity! 2

3 Lorentz Contraction Relativistic Effects Strange things effects are observed when objects are seen traveling close to the speed of light: Mass increases! Length decreases along the direction of motion! (Lorentz Contraction) The rate of passage of time slows down! (Time Dilation) Why can t we travel at or faster than the speed of light? A object observed to be traveling at the speed of light would be seen to have An infinite mass! A zero length! A rate of passage of time of zero = time stops! It is impossible to observe these things so it must be impossible to travel at or faster than c! The Equivalence Principle General Theory of Relativity (1915) Includes effects of accelerated motion which is the type of motion produced by gravity Is a theory of gravity! The effects of gravity and acceleration are identical 3

4 Newtonian Gravity: 3 dimension of space + 1 dimension of time Conclusion: strong gravitational fields produce the same relativistic effects seen for rapid motion e.g. time dilation! Einstein s Gravity: 4 dimensions of space-time Space-time is a 4-dimensional surface or hyperspace which is impossible to comprehend directly but can be thought of as representing the fabric of the Universe A 2D Analogy of 4D Spacetime Explains: The action of gravity across distance The shapes of planetary orbits they follow the curvature of spacetime around the Sun! Prediction: masses curve the fabric of spacetime around them e.g. a person on a trampoline Gravitational Bending of Light Experimental Confirmation of General Relativity Light follows the curvature of spacetime around a massive object! 4

5 Precession of the Orbit of Mercury Gravitational Time Dilation weaker gravity stronger gravity time slows Mercury s orbit is not stationary in space due to curvature of spacetime around the Sun Gravitational Redshift Gravitational Waves Ripples in spacetime caused by the acceleration of masses e.g. core collapse of massive a star light loses energy as it escapes from a source of gravity result: longer wavelengths Only prediction of General Relativity not measured Laser Interferometer Gravitational-Wave Observatory (LIGO) How it works! 5

6 The Formation of a Black Hole Each interferometer arm is 4 km long! Two observatories separated by 2000 miles! Able to confirm detections! A Black Hole is Highly Curved Spacetime The Structure of a Black Hole Schwartzschild Radius, R sh R sh = 3M km where: M = mass of black hole is solar masses Example: a 4 M Θ black hole has a radius of 3 x 4 = 12 km Common Misconception: Black holes gobble up all matter for 1000 s of light years around them! Not so! Spacetime highly curved close to hole but not far from it! Example: replace Sun with solar mass black hole planetary orbits would not change! 6

7 You can only be pulled into a black hole if you are very close to it! Properties of Singularities definition: non zero mass occupies zero volume a point of infinite density and gravity fabric of spacetime breaks a passage to parallel Universe? problem: laws of physics (even relativity) break down! have no way of predicting properties! Minimum stable orbit = 3R sh Problem: If singularities are places where the laws of physics do not apply, do black holes contradict the principle of relativity that the laws of physics are the same everywhere? Law of Cosmic Censorship Singularities are always surrounded by event horizons Blocks us from observing the unpredictable properties of singularities Black holes do not contradict relativity! Are any properties of black holes measurable? Yes! But only those properties that can be measured without electromagnetic radiation! 7

8 No Hair Theorem Only 3 properties can be measured for a black hole: mass charge rotation Mass Place a test probe of mass, M p in orbit around a black hole at a (safe!) chosen distance, a Measuring the orbital period, P of the probe will allow the mass of the black hole, M bh to be determined: P 2 = a 3 /(M bh + M p ) Charge A charged particle will be attracted or repelled by a black hole if it is charged! e - What is the charge of the hole? Negative! Rotation Frame dragging: close to a rotating black hole spacetime is dragged around Impossible to be still! Place probe in ergoregion to determine rotation! 8

9 Isolated black holes will distort the light from background objects Detecting Black Holes Isolated black holes very difficult to detect! Easier to detect black holes by the effect they have on neighboring matter e.g. a star Gravitational Microlensing Cygnus X-1 A very strong X-ray source in Cygnus the Swan General Relativity predicts that a black hole should magnify the light from a background star as it passes in front on it due to the distortion of space-time around it At the location of the X-ray source is a B0 I star Is this the source of the X-rays? A B0 star has T = 25,000 K Wien s Law T = 25,000 K λ max = UV The star is not hot enough to produce the X-rays! 9

10 Does the star have a companion? Spectrum? Single set of lines from B0 I star Lines are Doppler shifted back and forth with P = 5.6 days! A single-lined spectroscopic binary Conclusion: the companion must be dark and close Analyze orbit to obtain masses Mass B0 I star = 30 M Θ Mass companion = 3-7 M Θ Properties of Companion Emits little visible radiation Massive What could it be? A black hole! Cygnus X-1 is a Mass Transfer Binary Where do the X-rays come from? The X-rays come from the accretion disk of gas spiralling into the hole 10

11 Still some doubt due to uncertain mass of companion! If mass companion = 3 M Θ then could be a neutron star! Better examples of black hole candidates that cannot be neutron stars: V404 Cygni Mass companion > 6.26 M Θ A in Monoceros Mass companion > 3.2 M Θ IC 10 X-1 in the nearby galaxy IC 10 Mass companion M Θ Most massive known stellar mass black hole as of Fall 2007 Thought Experiment Release a probe and let it fall into a black hole from a safe distance! Equipment: a blue flashing light so you can follow its path a video camera to transmit back images Video Camera Images Results? 11

12 Gravitational Time Dilation Initially the probe will accelerate towards the hole However, as it approaches the event horizon it will appear to slow down due to the strong gravity! It will only reach the event horizon after an infinite amount of time where it will appear to be frozen in space! Gravitational Redshift As the probe approaches the event horizon the light from the probe is gravitationally redshifted from blue to green to yellow to red and will eventually become invisible as it shifts into non-visible wavelengths! It would disappear from view long before it reaches the event horizon! Tidal Forces Eventually the probe will break into pieces! As the probe approaches the hole, tidal forces will distort the shape of the probe! Wormholes A shortcut (tunnel) through hyperspace between two distant parts of the Universe allowing very rapid travel! Interstellar Travel Through Wormholes Big problem: we don t yet know how to create wormholes, and even if we did they would require enormous amounts of energy to form and keep open! 12

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

Survey of Astrophysics A110

Survey of Astrophysics A110 Black Holes Goals: Understand Special Relativity General Relativity How do we observe black holes. Black Holes A consequence of gravity Massive neutron (>3M ) cannot be supported by degenerate neutron

More information

ASTR 200 : Lecture 21. Stellar mass Black Holes

ASTR 200 : Lecture 21. Stellar mass Black Holes 1 ASTR 200 : Lecture 21 Stellar mass Black Holes High-mass core collapse Just as there is an upper limit to the mass of a white dwarf (the Chandrasekhar limit), there is an upper limit to the mass of a

More information

Black Holes -Chapter 21

Black Holes -Chapter 21 Black Holes -Chapter 21 The most massive stellar cores If the core is massive enough (~3 M ; total initial mass of star > 25 M or so), even neutron degeneracy pressure can be overwhelmed by gravity. A

More information

22. Black Holes. Relativistic Length Contraction. Relativistic Time Dilation

22. Black Holes. Relativistic Length Contraction. Relativistic Time Dilation 22. Black Holes Einstein s Special Theory of Relativity Einstein s General Theory of Relativity Black holes exist in some binary star systems Supermassive black holes at of galaxy centers Two properties

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

Einstein s Relativity and Black Holes

Einstein s Relativity and Black Holes Einstein s Relativity and Black Holes Guiding Questions 1. What are the two central ideas behind Einstein s special theory of relativity? 2. How do astronomers search for black holes? 3. In what sense

More information

Black Holes. Over the top? Black Holes. Gravity s Final Victory. Einstein s Gravity. Near Black holes escape speed is greater than the speed of light

Black Holes. Over the top? Black Holes. Gravity s Final Victory. Einstein s Gravity. Near Black holes escape speed is greater than the speed of light Black Holes Over the top? What if the remnant core is very massive? M core > 2-3 M sun (original star had M > 18 M sun ) Neutron degeneracy pressure fails. Nothing can stop gravitational collapse. Collapses

More information

GR and Spacetime 3/20/14. Joys of Black Holes. Compact Companions in Binary Systems. What do we mean by the event horizon of a black hole?

GR and Spacetime 3/20/14. Joys of Black Holes. Compact Companions in Binary Systems. What do we mean by the event horizon of a black hole? ASTR 1040: Stars & Galaxies Prof. Juri Toomre TA: Ryan Orvedahl Lecture 20 Thur 20 Mar 2014 zeus.colorado.edu/astr1040-toomre Tycho Brahe SNR (1572) Joys of Black Holes Black holes, their general properties,

More information

Black Holes, or the Monster at the Center of the Galaxy

Black Holes, or the Monster at the Center of the Galaxy Black Holes, or the Monster at the Center of the Galaxy Learning Objectives! How do black holes with masses a few times that of our Sun form? How can we observe such black holes?! Where and how might you

More information

Test #3 Next Tuesday, Nov. 8 Bring your UNM ID! Bring two number 2 pencils. Announcements. Review for test on Monday, Nov 7 at 3:25pm

Test #3 Next Tuesday, Nov. 8 Bring your UNM ID! Bring two number 2 pencils. Announcements. Review for test on Monday, Nov 7 at 3:25pm Test #3 Next Tuesday, Nov. 8 Bring your UNM ID! Bring two number 2 pencils Announcements Review for test on Monday, Nov 7 at 3:25pm Neutron Star - Black Hole merger Review for Test #3 Nov 8 Topics: Stars

More information

Einstein s Gravity. Understanding space-time and the gravitational effects of mass

Einstein s Gravity. Understanding space-time and the gravitational effects of mass Einstein s Gravity Understanding space-time and the gravitational effects of mass Albert Einstein (1879-1955) One of the iconic figures of the 20 th century, Einstein revolutionized our understanding of

More information

General Relativity. In GR, mass (or energy) warps the spacetime fabric of space.

General Relativity. In GR, mass (or energy) warps the spacetime fabric of space. General Relativity Einstein s theory of General Relativity is a theory of gravity The basic idea is to drop Newton s idea of a mysterious force between masses and replace it with the 4-dimensional SpaceTime

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

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

ASTR 200 : Lecture 31. More Gravity: Tides, GR, and Gravitational Waves

ASTR 200 : Lecture 31. More Gravity: Tides, GR, and Gravitational Waves ASTR 200 : Lecture 31 More Gravity: Tides, GR, and Gravitational Waves 1 Topic One : Tides Differential tidal forces on the Earth. 2 How do tides work???? Think about 3 billiard balls sitting in space

More information

ASTR 200 : Lecture 30. More Gravity: Tides, GR, and Gravitational Waves

ASTR 200 : Lecture 30. More Gravity: Tides, GR, and Gravitational Waves ASTR 200 : Lecture 30 More Gravity: Tides, GR, and Gravitational Waves 1 Topic One : Tides Differential tidal forces on the Earth. 2 How do tides work???? Think about 3 billiard balls sitting in space

More information

Space and Time Before Einstein. The Problem with Light. Admin. 11/2/17. Key Concepts: Lecture 28: Relativity

Space and Time Before Einstein. The Problem with Light. Admin. 11/2/17. Key Concepts: Lecture 28: Relativity Admin. 11/2/17 1. Class website http://www.astro.ufl.edu/~jt/teaching/ast1002/ 2. Optional Discussion sections: Tue. ~11.30am (period 5), Bryant 3; Thur. ~12.30pm (end of period 5 and period 6), start

More information

Lecture 18 : Black holes. Astronomy 111

Lecture 18 : Black holes. Astronomy 111 Lecture 18 : Black holes Astronomy 111 Gravity's final victory A star more massive than about 18 M sun would leave behind a post-supernova core this is larger than 2-3 M sun :Neutron degeneracy pressure

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

Lecture 23: Black Holes Readings: Sections 24-3, 24-5 through 24-8

Lecture 23: Black Holes Readings: Sections 24-3, 24-5 through 24-8 Lecture 23: Black Holes Readings: Sections 24-3, 24-5 through 24-8 Key Ideas Black Holes are totally collapsed objects Gravity so strong not even light can escape Predicted by General Relativity Schwarzschild

More information

Black Holes. Class 17 Prof J. Kenney June 19, 2018

Black Holes. Class 17 Prof J. Kenney June 19, 2018 Black Holes Class 17 Prof J. Kenney June 19, 2018 basic structure of (non-rotating) black hole basic structure of (non-rotating) black hole SINGULARITY: all the mass of the black hole is crushed to incredibly

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

Black Holes in Terms of Escape Velocity. Agenda for Ast 309N, Nov. 27. How Big is the Event Horizon? The Anatomy of a (Simple) Black Hole

Black Holes in Terms of Escape Velocity. Agenda for Ast 309N, Nov. 27. How Big is the Event Horizon? The Anatomy of a (Simple) Black Hole Agenda for Ast 309N, Nov. 27 Black Holes in Terms of Escape Velocity Optional HW 3 - due now; Quiz 8 Thursday Next week: repeat survey (Tues), Exam 3 (Thurs) Feedback on black hole index cards Black hole

More information

Review Special Relativity. February 3, Absolutes of Relativity. Key Ideas of Special Relativity. Path of Ball in a Moving Train

Review Special Relativity. February 3, Absolutes of Relativity. Key Ideas of Special Relativity. Path of Ball in a Moving Train February 3, 2009 Review Special Relativity General Relativity Key Ideas of Special Relativity No material object can travel faster than light If you observe something moving near light speed: Its time

More information

Astronomy 1 Fall 2016

Astronomy 1 Fall 2016 Astronomy 1 Fall 2016 Lecture 14; November 10, 2016 Previously on Astro 1 Late evolution and death of intermediate-mass stars (about 0.4 M to about 4 M ): red giant when shell hydrogen fusion begins, a

More information

NEUTRON STARS, GAMMA RAY BURSTS, and BLACK HOLES (chap. 22 in textbook)

NEUTRON STARS, GAMMA RAY BURSTS, and BLACK HOLES (chap. 22 in textbook) NEUTRON STARS, GAMMA RAY BURSTS, and BLACK HOLES (chap. 22 in textbook) Neutron Stars For carbon detonation SN probably no remnant For core-collapse SN remnant is a neutron-degenerate core neutron star

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

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

7/5. Consequences of the principle of equivalence (#3) 1. Gravity is a manifestation of the curvature of space.

7/5. Consequences of the principle of equivalence (#3) 1. Gravity is a manifestation of the curvature of space. 7/5 Consequences of the principle of equivalence (#3) 1. Gravity is a manifestation of the curvature of space. Follow the path of a light pulse in an elevator accelerating in gravityfree space. The dashed

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

8/30/2010. Classifying Stars. Classifying Stars. Classifying Stars

8/30/2010. Classifying Stars. Classifying Stars. Classifying Stars Classifying Stars In the early 1900s, Ejnar Hertzsprung and Henry Russell made some important observations. They noticed that, in general, stars with higher temperatures also have brighter absolute magnitudes.

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

Chapter S3 Spacetime and Gravity. Agenda. Distinguishing Crackpots

Chapter S3 Spacetime and Gravity. Agenda. Distinguishing Crackpots Chapter S3 Spacetime and Gravity Agenda Announce: Online Quizzes Observations Extra Credit Lecture Distinguishing Crackpot/Genuine Science Review of Special Relativity General Relativity Distinguishing

More information

The interpretation is that gravity bends spacetime and that light follows the curvature of space.

The interpretation is that gravity bends spacetime and that light follows the curvature of space. 7/8 General Theory of Relativity GR Two Postulates of the General Theory of Relativity: 1. The laws of physics are the same in all frames of reference. 2. The principle of equivalence. Three statements

More information

10/25/2010. Stars, Galaxies & the Universe Announcements. Stars, Galaxies & the Universe Lecture Outline. Reading Quiz #9 Wednesday (10/27)

10/25/2010. Stars, Galaxies & the Universe Announcements. Stars, Galaxies & the Universe Lecture Outline. Reading Quiz #9 Wednesday (10/27) Stars, Galaxies & the Universe Announcements Reading Quiz #9 Wednesday (10/27) HW#8 in ICON due Friday (10/29) by 5 pm - available Wednesday 1 Stars, Galaxies & the Universe Lecture Outline 1. Black Holes

More information

Centers of Galaxies. = Black Holes and Quasars

Centers of Galaxies. = Black Holes and Quasars Centers of Galaxies = Black Holes and Quasars Models of Nature: Kepler Newton Einstein (Special Relativity) Einstein (General Relativity) Motions under influence of gravity [23] Kepler The planets move

More information

2) On a Hertzsprung-Russell diagram, where would you find red giant stars? A) upper right B) lower right C) upper left D) lower left

2) On a Hertzsprung-Russell diagram, where would you find red giant stars? A) upper right B) lower right C) upper left D) lower left Multiple choice test questions 2, Winter Semester 2015. Based on parts covered after mid term. Essentially on Ch. 12-2.3,13.1-3,14,16.1-2,17,18.1-2,4,19.5. You may use a calculator and the useful formulae

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

18.3 Black Holes: Gravity's Ultimate Victory

18.3 Black Holes: Gravity's Ultimate Victory 18.3 Black Holes: Gravity's Ultimate Victory Our goals for learning: What is a black hole? What would it be like to visit a black hole? Do black holes really exist? What is a black hole? Gravity, Newton,

More information

Syllabus and Schedule for ASTRO 210 (Black Holes)

Syllabus and Schedule for ASTRO 210 (Black Holes) Black Holes Syllabus and Schedule for ASTRO 210 (Black Holes) The syllabus and schedule for this class are located at: http://chartasg.people.cofc.edu/chartas/teaching.html Gravity is Universal Gravity

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

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

Astronomy 182: Origin and Evolution of the Universe

Astronomy 182: Origin and Evolution of the Universe Astronomy 182: Origin and Evolution of the Universe Prof. Josh Frieman Lecture 6 Oct. 28, 2015 Today Wrap up of Einstein s General Relativity Curved Spacetime Gravitational Waves Black Holes Relativistic

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

Gravity: What s the big attraction? Dan Wilkins Institute of Astronomy

Gravity: What s the big attraction? Dan Wilkins Institute of Astronomy Gravity: What s the big attraction? Dan Wilkins Institute of Astronomy Overview What is gravity? Newton and Einstein What does gravity do? Extreme gravity The true power of gravity Getting things moving

More information

What is a Black Hole?

What is a Black Hole? What is a Black Hole? Robert H. Gowdy Virginia Commonwealth University December 2016 Bob G (VCU) Black Holes December 2016 1 / 29 Black Holes Bob G (VCU) Black Holes December 2016 2 / 29 Overview Spacetime

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

A100 Exploring the Universe: Black holes. Martin D. Weinberg UMass Astronomy

A100 Exploring the Universe: Black holes. Martin D. Weinberg UMass Astronomy A100 Exploring the Universe: Black holes Martin D. Weinberg UMass Astronomy weinberg@astro.umass.edu October 30, 2014 Read: S2, S3, Chap 18 10/30/14 slide 1 Sizes of s The solar neighborhood visualized!

More information

How Do Stars Appear from Earth?

How Do Stars Appear from Earth? How Do Stars Appear from Earth? Magnitude: the brightness a star appears to have from Earth Apparent Magnitude depends on 2 things: (actual intrinsic brightness) The color of a star is related to its temperature:

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

Neutron Stars. Neutron Stars and Black Holes. The Crab Pulsar. Discovery of Pulsars. The Crab Pulsar. Light curves of the Crab Pulsar.

Neutron Stars. Neutron Stars and Black Holes. The Crab Pulsar. Discovery of Pulsars. The Crab Pulsar. Light curves of the Crab Pulsar. Chapter 11: Neutron Stars and Black Holes A supernova explosion of an M > 8 M sun star blows away its outer layers. Neutron Stars The central core will collapse into a compact object of ~ a few M sun.

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

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

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

1. (15.1) What are the approximate mass and radius of a white dwarf compared with those of the Sun?

1. (15.1) What are the approximate mass and radius of a white dwarf compared with those of the Sun? SUMMARY White dwarfs, neutron stars, and black holes are the remnants of dead stars. A white dwarf forms when a low mass star expels its outer layers to form a planetary nebula shell and leaves its hot

More information

GENERAL RELATIVITY. The presence of matter affects 4-space.

GENERAL RELATIVITY. The presence of matter affects 4-space. GENERAL RELATIVITY Whereas Special Relativity is the study of constant velocity motion, General Relativity is associated with situations in which accelerations exist. As gravitation produces acceleration,

More information

Astronomy 421. Lecture 24: Black Holes

Astronomy 421. Lecture 24: Black Holes Astronomy 421 Lecture 24: Black Holes 1 Outline General Relativity Equivalence Principle and its Consequences The Schwarzschild Metric The Kerr Metric for rotating black holes Black holes Black hole candidates

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 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

SPECIAL RELATIVITY! (Einstein 1905)!

SPECIAL RELATIVITY! (Einstein 1905)! SPECIAL RELATIVITY! (Einstein 1905)! Motivations:! Explaining the results of the Michelson-Morley! experiment without invoking a force exerted! on bodies moving through the aether.! Make the equations

More information

Astronomy 122 Outline

Astronomy 122 Outline Astronomy 122 Outline This Class (Lecture 19): Black Holes Next Class: The Milkyway Last Nightlab tonight! HW7 due on Friday. Mar Lecture report due in discussion class on April 5 th th. Nightlab report

More information

Special theory of relativity

Special theory of relativity Announcements l CAPA #9 due Tuesday April 1 l Mastering Physics Chapter 35 due April 1 l Average on exam #2 is 26/40 l For the sum of the first two exams (80 points); l >=67 4.0 l 61-66 3.5 l 50-60 3.0

More information

Chapter 33 The History of a Star. Introduction. Radio telescopes allow us to look into the center of the galaxy. The milky way

Chapter 33 The History of a Star. Introduction. Radio telescopes allow us to look into the center of the galaxy. The milky way Chapter 33 The History of a Star Introduction Did you read chapter 33 before coming to class? A. Yes B. No You can see about 10,000 stars with the naked eye. The milky way Radio telescopes allow us to

More information

Black Holes. By Alexander Bamert and Jay Bober

Black Holes. By Alexander Bamert and Jay Bober Black Holes By Alexander Bamert and Jay Bober History In 1939, J. Robert Oppenheimer and Hartland Snyder calculated the first models of neutron stars Proceeded to question what would happen when a star

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

Stellar Evolution: Outline

Stellar Evolution: Outline Stellar Evolution: Outline Interstellar Medium (dust) Hydrogen and Helium Small amounts of Carbon Dioxide (makes it easier to detect) Massive amounts of material between 100,000 and 10,000,000 solar masses

More information

29:50 Stars, Galaxies, and the Universe Second Hour Exam November 10, 2010 Form A

29:50 Stars, Galaxies, and the Universe Second Hour Exam November 10, 2010 Form A 29:50 Stars, Galaxies, and the Universe Second Hour Exam November 10, 2010 Form A There are 20 questions (Note: There will be 32 on the real thing). Read each question and all of the choices before choosing.

More information

Formation of the Universe & What is in Space? The Big Bang Theory and components of the Universe

Formation of the Universe & What is in Space? The Big Bang Theory and components of the Universe Formation of the Universe & What is in Space? The Big Bang Theory and components of the Universe The Big Bang Theory The Big Bang Theory The Big Bang Theory is the most widely accepted scientific explanation

More information

Homework 6 Name: Due Date: June 9, 2008

Homework 6 Name: Due Date: June 9, 2008 Homework 6 Name: Due Date: June 9, 2008 1. Where in the universe does the general expansion occur? A) everywhere in the universe, including our local space upon Earth, the solar system, our galaxy and

More information

A100H Exploring the Universe: Black holes. Martin D. Weinberg UMass Astronomy

A100H Exploring the Universe: Black holes. Martin D. Weinberg UMass Astronomy A100H Exploring the Universe: Black holes Martin D. Weinberg UMass Astronomy astron100h-mdw@courses.umass.edu March 22, 2016 Read: S2, S3, Chap 18 03/22/16 slide 1 Exam #2: March 29 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

ASTR 101 General Astronomy: Stars & Galaxies. NEXT Tuesday 4/4 MIDTERM #2

ASTR 101 General Astronomy: Stars & Galaxies. NEXT Tuesday 4/4 MIDTERM #2 ASTR 101 General Astronomy: Stars & Galaxies NEXT Tuesday 4/4 MIDTERM #2 The Stellar Graveyard What s In The Stellar Graveyard? Lower mass stars (M< 8M sun ) à white dwarfs Gravity vs. electron degeneracy

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

Wallace Hall Academy

Wallace Hall Academy Wallace Hall Academy CfE Higher Physics Unit 1 - Universe Notes Name 1 Newton and Gravity Newton s Thought Experiment Satellite s orbit as an Application of Projectiles Isaac Newton, as well as giving

More information

Class 16. Prof J. Kenney October 31, Relativity

Class 16. Prof J. Kenney October 31, Relativity Class 16 Prof J. Kenney October 31, 2016 Relativity Length contraction (moving sticks are shorter) A measuring stick at rest has a length Lo. When it is propelled at velocity v, it has a shorter length

More information

Cosmology, Galaxies, and Stars OUR VISIBLE UNIVERSE

Cosmology, Galaxies, and Stars OUR VISIBLE UNIVERSE Cosmology, Galaxies, and Stars OUR VISIBLE UNIVERSE Cosmology Cosmology is the study of the universe; its nature, origin and evolution. General Relativity is the mathematical basis of cosmology from which

More information

Relativity. Class 16 Prof J. Kenney June 18, boss

Relativity. Class 16 Prof J. Kenney June 18, boss Relativity Class 16 Prof J. Kenney June 18, 2018 boss Length contraction (moving sticks are shorter) A measuring stick at rest has a length Lo. When it is propelled at velocity v, it has a shorter length

More information

Astronomy in the news? GOCE crash?

Astronomy in the news? GOCE crash? Monday, November 11, 2013 Exam 4 Friday. Review sheet posted. Review session Thursday, 5 6 PM, WRW 102 Reading: Chapter 9: all except 9.6.3, 9.6.4 Chapter 10, Sections 10.1-10.6, 10.9 Astronomy in the

More information

Gravity Waves and Black Holes

Gravity Waves and Black Holes Gravity Waves and Black Holes Mike Whybray Orwell Astronomical Society (Ipswich) 14 th March 2016 Overview Introduction to Special and General Relativity The nature of Black Holes What to expect when Black

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

Chapter 21 Astronomy Today 7th Edition Chaisson/McMillan

Chapter 21 Astronomy Today 7th Edition Chaisson/McMillan Lecture Outlines Chapter 21 Astronomy Today 7th Edition Chaisson/McMillan Chapter 21 Stellar Explosions Units of Chapter 21 21.1 Life after Death for White Dwarfs 21.2 The End of a High-Mass Star 21.3

More information

Accretion Disks. Review: Stellar Remnats. Lecture 12: Black Holes & the Milky Way A2020 Prof. Tom Megeath 2/25/10. Review: Creating Stellar Remnants

Accretion Disks. Review: Stellar Remnats. Lecture 12: Black Holes & the Milky Way A2020 Prof. Tom Megeath 2/25/10. Review: Creating Stellar Remnants Lecture 12: Black Holes & the Milky Way A2020 Prof. Tom Megeath Review: Creating Stellar Remnants Binaries may be destroyed in white dwarf supernova Binaries be converted into black holes Review: Stellar

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

Announcements. Lecture 6. General Relativity. From before. Space/Time - Energy/Momentum

Announcements. Lecture 6. General Relativity. From before. Space/Time - Energy/Momentum Announcements 2402 Lab will be started next week Lab manual will be posted on the course web today Lab Scheduling is almost done!! HW: Chapter.2 70, 75, 76, 87, 92, 97*, 99, 104, 111 1 st Quiz: 9/18 (Ch.2)

More information

Astronomy Hour Exam 2 March 10, 2011 QUESTION 1: The half-life of Ra 226 (radium) is 1600 years. If you started with a sample of 100 Ra 226

Astronomy Hour Exam 2 March 10, 2011 QUESTION 1: The half-life of Ra 226 (radium) is 1600 years. If you started with a sample of 100 Ra 226 Astronomy 101.003 Hour Exam 2 March 10, 2011 QUESTION 1: The half-life of Ra 226 (radium) is 1600 years. If you started with a sample of 100 Ra 226 atoms, approximately how many Ra 226 atoms would be left

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

Lecture PowerPoints. Chapter 33 Physics: Principles with Applications, 7 th edition Giancoli

Lecture PowerPoints. Chapter 33 Physics: Principles with Applications, 7 th edition Giancoli Lecture PowerPoints Chapter 33 Physics: Principles with Applications, 7 th edition Giancoli This work is protected by United States copyright laws and is provided solely for the use of instructors in teaching

More information

Energy Source for Active Galactic Nuclei

Energy Source for Active Galactic Nuclei Quasars Quasars are small, extremely luminous, extremely distant galactic nuclei Bright radio sources Name comes from Quasi-Stellar Radio Source, as they appeared to be stars! Can have clouds of gas near

More information

Mr Green sees the shorter, straight, green path and Mr. Red sees the longer, curved, red path.

Mr Green sees the shorter, straight, green path and Mr. Red sees the longer, curved, red path. Mr Green sees the shorter, straight, green path and Mr. Red sees the longer, curved, red path. In an accelerated frame, time runs slow compared to a non-accelerated frame. The Equivalence Principle tells

More information

Chapter S3 Spacetime and Gravity Pearson Education, Inc.

Chapter S3 Spacetime and Gravity Pearson Education, Inc. Chapter S3 Spacetime and Gravity What are the major ideas of general relativity? Spacetime Special relativity showed that space and time are not absolute. Instead, they are inextricably linked in a four-dimensional

More information

Outline. General Relativity. Black Holes as a consequence of GR. Gravitational redshift/blueshift and time dilation Curvature Gravitational Lensing

Outline. General Relativity. Black Holes as a consequence of GR. Gravitational redshift/blueshift and time dilation Curvature Gravitational Lensing Outline General Relativity Gravitational redshift/blueshift and time dilation Curvature Gravitational Lensing Black Holes as a consequence of GR Waste Disposal It is decided that Earth will get rid of

More information

Looking for ripples of gravity with LIGO. Phil Willems, California Institute of Technology. LIGO Laboratory 1 G G

Looking for ripples of gravity with LIGO. Phil Willems, California Institute of Technology. LIGO Laboratory 1 G G Looking for ripples of gravity with LIGO Phil Willems, California Institute of Technology LIGO Laboratory 1 LIGO: -an experiment to measure gravitational waves from the cosmos LIGO Laboratory 2 Laser Interferometer

More information

25.2 Stellar Evolution. By studying stars of different ages, astronomers have been able to piece together the evolution of a star.

25.2 Stellar Evolution. By studying stars of different ages, astronomers have been able to piece together the evolution of a star. 25.2 Stellar Evolution By studying stars of different ages, astronomers have been able to piece together the evolution of a star. Star Birth The birthplaces of stars are dark, cool interstellar clouds,

More information

GraspIT Questions AQA GCSE Physics Space physics

GraspIT Questions AQA GCSE Physics Space physics A. Solar system: stability of orbital motions; satellites (physics only) 1. Put these astronomical objects in order of size from largest to smallest. (3) Fill in the boxes in the correct order. the Moon

More information

Notes for Wednesday, July 16; Sample questions start on page 2 7/16/2008

Notes for Wednesday, July 16; Sample questions start on page 2 7/16/2008 Notes for Wednesday, July 16; Sample questions start on page 2 7/16/2008 Wed, July 16 MW galaxy, then review. Start with ECP3Ch14 2 through 8 Then Ch23 # 8 & Ch 19 # 27 & 28 Allowed Harlow Shapely to locate

More information

Chapter 19 Galaxies. Hubble Ultra Deep Field: Each dot is a galaxy of stars. More distant, further into the past. halo

Chapter 19 Galaxies. Hubble Ultra Deep Field: Each dot is a galaxy of stars. More distant, further into the past. halo Chapter 19 Galaxies Hubble Ultra Deep Field: Each dot is a galaxy of stars. More distant, further into the past halo disk bulge Barred Spiral Galaxy: Has a bar of stars across the bulge Spiral Galaxy 1

More information

8. The Expanding Universe, Revisited

8. The Expanding Universe, Revisited 8. The Expanding Universe, Revisited A1143: History of the Universe, Autumn 2012 Now that we have learned something about Einstein s theory of gravity, we are ready to revisit what we have learned about

More information

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 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

More information

THE ORIGIN OF THE UNIVERSE AND BLACK HOLES

THE ORIGIN OF THE UNIVERSE AND BLACK HOLES THE ORIGIN OF THE UNIVERSE AND BLACK HOLES WHAT IS COSMOGONY? Cosmogony (or cosmogeny) is any model explaining the origin of the universe. Cosmogony = Coming into existence WHAT IS COSMOLOGY Cosmology

More information