Relativistic Astrophysics Neutron Stars, Black Holes & Grav. W. ... A brief description of the course
|
|
|
- Diana Booth
- 6 years ago
- Views:
Transcription
1 Relativistic Astrophysics Neutron Stars, Black Holes & Grav. Waves... A brief description of the course May 2, 2009
2 Structure of the Course Introduction to General Theory of Relativity (2-3 weeks) Gravitational Collapse (1 week) Neutron Stars (2-3 weeks) Black Holes (2-3 weeks) Gravitational Waves (2-3 weeks)
3 Introduction to General Theory of Relativity Short Introduction to Tensors What is General Relativity and Einstein s equations Three solutions of Einstein s equations with astrophysical interest (Schwarschild, Kerr, TOV) Orbits in the vicinity of black-holes
4 Gravitational Collapse A typical supernova occurs when the core of a massive star runs out of nuclear fuel and collapses under its own gravity to form an ultra-dense object known as a neutron star. The newborn neutron star compresses and then rebounds, triggering a shock wave that ploughs through the star s gaseous outer layers and blows the star to smithereens. Figure: Supernova explosion Figure: Crab Nebula Figure: Supernova 1987a, photo taken by the Hubble telescope in 1995
5 Gravitational Collapse Supernovae result from the explosive death of a star and are classified as two types. Type Ia supernovae occur in binary star systems in which gas from one star falls onto a white dwarf with a mass close to the Chandrasekhar critical mass and causes it to explode. The explosion is caused by the ignition of runaway thermo-nuclear reactions under degenerate matter conditions. Type II supernovae occur in stars at least ten times more massive than our Sun, which suffer runaway thermo-nuclear reactions at the end of their lives, leading to explosions. Such explosions can be either total (no solid remnant) or may leave behind a rapidly spinning neutron star (a pulsar) or a black hole.
6 Neutron Stars A neutron star is a type of remnant that can result from the gravitational collapse of a massive star during a Type II, Type Ib or Type Ic supernova event. Such stars are composed almost entirely of neutrons. Neutron stars are very hot and are supported against further collapse because of the Pauli exclusion principle. This principle states that no two neutrons (or any other fermionic particle) can occupy the same quantum state simultaneously. A typical NS has a mass between M, with a corresponding radius of 9-15 km and central densities around gr/cm 3. Figure: Pulsar Figure: LMXB Figure: Magnetar
7 Neutron Stars Equilibrium configurations in GR How to construct a relativistic star White Dwarf Stars Neutron Stars pure neutron stars more complicated equation of state maximum mass of NS rotation, pulsars Magnetic fields on NS & Magnetars Binary Pulsars Low-mass X-ray binaries (LMXB) Intermediate-mass X-ray binaries (IMXB) High-mass X-ray binaries (HMXB) Accretion-powered pulsar ( X-ray pulsar ) Exotic Stars
8 Neutron Stars Equilibrium configurations in GR How to construct a relativistic star White Dwarf Stars Neutron Stars pure neutron stars more complicated equation of state maximum mass of NS rotation, pulsars Magnetic fields on NS & Magnetars Binary Pulsars Low-mass X-ray binaries (LMXB) Intermediate-mass X-ray binaries (IMXB) High-mass X-ray binaries (HMXB) Accretion-powered pulsar ( X-ray pulsar ) Exotic Stars
9 Neutron Stars Equilibrium configurations in GR How to construct a relativistic star White Dwarf Stars Neutron Stars pure neutron stars more complicated equation of state maximum mass of NS rotation, pulsars Magnetic fields on NS & Magnetars Binary Pulsars Low-mass X-ray binaries (LMXB) Intermediate-mass X-ray binaries (IMXB) High-mass X-ray binaries (HMXB) Accretion-powered pulsar ( X-ray pulsar ) Exotic Stars
10 Neutron Stars Equilibrium configurations in GR How to construct a relativistic star White Dwarf Stars Neutron Stars pure neutron stars more complicated equation of state maximum mass of NS rotation, pulsars Magnetic fields on NS & Magnetars Binary Pulsars Low-mass X-ray binaries (LMXB) Intermediate-mass X-ray binaries (IMXB) High-mass X-ray binaries (HMXB) Accretion-powered pulsar ( X-ray pulsar ) Exotic Stars
11 Neutron Stars Equilibrium configurations in GR How to construct a relativistic star White Dwarf Stars Neutron Stars pure neutron stars more complicated equation of state maximum mass of NS rotation, pulsars Magnetic fields on NS & Magnetars Binary Pulsars Low-mass X-ray binaries (LMXB) Intermediate-mass X-ray binaries (IMXB) High-mass X-ray binaries (HMXB) Accretion-powered pulsar ( X-ray pulsar ) Exotic Stars
12 Neutron Stars Equilibrium configurations in GR How to construct a relativistic star White Dwarf Stars Neutron Stars pure neutron stars more complicated equation of state maximum mass of NS rotation, pulsars Magnetic fields on NS & Magnetars Binary Pulsars Low-mass X-ray binaries (LMXB) Intermediate-mass X-ray binaries (IMXB) High-mass X-ray binaries (HMXB) Accretion-powered pulsar ( X-ray pulsar ) Exotic Stars
13 Black Holes Black holes are among the most intriguing objects in modern physics. They power quasars and other active galactic nuclei and also provide key insights into quantum gravity. We will review the observational evidence for black holes and briefly discuss some of their properties. We will also issues related to black-hole thermodynamics. Figure: BH Spacetime Figure: BHs have no hair Figure: BH in action
14 Black Holes What are the black holes according to GR Observational evidence for BHs The maximum mass of neutron stars Observational signatures of black holes Supermassive black holes in galactic nuclei Black holes in x-ray binaries Conclusive evidence for black holes Quantum Black Holes
15 Gravitational Waves Gravitational forces cannot be transmitted or communicated faster than light. This means that when the gravitational field of an object changes, the information about these changes will take a finite time to reach other objects. These ripples are called gravitational radiation or gravitational waves. Figure: Gravitational Waves Figure: Merging Neutron Stars Figure: Merging Neutron Stars
16 Gravitational Waves What are the gravitational waves How do they produced Astrophysical Sources of GWs Binary Systems Supernova Collapse Isolated Neutron Stars Early Universe Detection of Gravitational Waves Figure: Schematic GW Detector Figure: Virgo & LISA
17 Gravitational Waves What are the gravitational waves How do they produced Astrophysical Sources of GWs Binary Systems Supernova Collapse Isolated Neutron Stars Early Universe Detection of Gravitational Waves Figure: Schematic GW Detector Figure: Virgo & LISA
18 Gravitational Waves What are the gravitational waves How do they produced Astrophysical Sources of GWs Binary Systems Supernova Collapse Isolated Neutron Stars Early Universe Detection of Gravitational Waves Figure: Schematic GW Detector Figure: Virgo & LISA
19 Gravitational Waves What are the gravitational waves How do they produced Astrophysical Sources of GWs Binary Systems Supernova Collapse Isolated Neutron Stars Early Universe Detection of Gravitational Waves Figure: Schematic GW Detector Figure: Virgo & LISA
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
Planetary Nebulae evolve to White Dwarf Stars
Planetary Nebulae evolve to White Dwarf Stars 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
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
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
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
Wednesday, February 3, 2016 First exam Friday. First Sky Watch Due (typed, 8.5x11 paper). Review sheet posted. Review session Thursday, 4:30 5:30 PM
Wednesday, February 3, 2016 First exam Friday. First Sky Watch Due (typed, 8.5x11 paper). Review sheet posted. Review session Thursday, 4:30 5:30 PM RLM 15.216B (Backup RLM 15.202A) Reading: Chapter 6
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 ~
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
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
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
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
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
Gravitational Wave Astronomy the sound of spacetime. Marc Favata Kavli Institute for Theoretical Physics
Gravitational Wave Astronomy the sound of spacetime Marc Favata Kavli Institute for Theoretical Physics What are gravitational waves? Oscillations in the gravitational field ripples in the curvature of
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
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
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?
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
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
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
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
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
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
Life and Death of a Star 2015
Life and Death of a Star 2015 Name Date 1. In the main-sequence, the core is slowly shrinking because A. the mass of the star is slowly increasing B. hydrogen fusing to helium makes the core more dense
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
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
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
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
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.
Life and Death of a Star. Chapters 20 and 21
Life and Death of a Star Chapters 20 and 21 90 % of a stars life Most stars spend most of their lives on the main sequence. A star like the Sun, for example, after spending a few tens of millions of years
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
Introductory Astrophysics A113. Death of Stars. Relation between the mass of a star and its death White dwarfs and supernovae Enrichment of the ISM
Goals: Death of Stars Relation between the mass of a star and its death White dwarfs and supernovae Enrichment of the ISM Low Mass Stars (M
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
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
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$
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
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
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
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
X-Ray Spectroscopy of Supernova Remnants. Introduction and Background:
X-Ray Spectroscopy of Supernova Remnants Introduction and Background: RCW 86 (Chandra, XMM-Newton) RCW 86 is a supernova remnant that was created by the destruction of a star approximately two thousand
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
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
The electrons then interact with the surrounding medium, heat it up, and power the light curve. 56 Ni 56 Co + e (1.72 MeV) half life 6.
Supernovae The spectra of supernovae fall into many categories (see below), but beginning in about 1985, astronomers recognized that there were physically, only two basic types of supernovae: Type Ia and
Chapter 15. Supernovae Classification of Supernovae
Chapter 15 Supernovae Supernovae represent the catastrophic death of certain stars. They are among the most violent events in the Universe, typically producing about 10 53 erg, with a large fraction of
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
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
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
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
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
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
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
Black Holes ASTR 2110 Sarazin. Calculation of Curved Spacetime near Merging Black Holes
Black Holes ASTR 2110 Sarazin Calculation of Curved Spacetime near Merging Black Holes Test #2 Monday, November 13, 11-11:50 am Ruffner G006 (classroom) Bring pencils, paper, calculator You may not consult
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
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
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
GRAVITATIONAL COLLAPSE
GRAVITATIONAL COLLAPSE Landau and Chandrasekhar first realised the importance of General Relativity for Stars (1930). If we increase their mass and/or density, the effects of gravitation become increasingly
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:
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
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
Brock University. Test 1, February, 2017 Number of pages: 9 Course: ASTR 1P02 Number of Students: 480 Date of Examination: February 6, 2017
Brock University Test 1, February, 2017 Number of pages: 9 Course: ASTR 1P02 Number of Students: 480 Date of Examination: February 6, 2017 Number of hours: 50 min Time of Examination: 18:00 18:50 Instructor:
Neutron Stars. But what happens to the super-dense core? It faces two possible fates:
Neutron Stars When a massive star runs out of fuel, its core collapses from the size of the Earth to a compact ball of neutrons just ten miles or so across. Material just outside the core falls onto this
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!
Ch. 29 The Stars Stellar Evolution
Ch. 29 The Stars 29.3 Stellar Evolution Basic Structure of Stars Mass effects The more massive a star is, the greater the gravity pressing inward, and the hotter and more dense the star must be inside
The Death of Stars. Ra Inta, Texas Tech University
The Death of Stars Ra Inta, Texas Tech University I: Stellar Evolution ESO - https://www.eso.org/public/images/eso0728c/ Burning stages of a 25 M star Fuel Product(s) H He He C, O C Ne, Na, Mg, Al Ne O,
HPC in Physics. (particularly astrophysics) Reuben D. Budiardja Scientific Computing National Institute for Computational Sciences
HPC in Physics (particularly astrophysics) Reuben D. Budiardja Scientific Computing National Institute for Computational Sciences 1 Gravitational Wave Einstein s Unfinished Symphony Marcia Bartuciak Predicted
Guiding Questions. The Deaths of Stars. Pathways of Stellar Evolution GOOD TO KNOW. Low-mass stars go through two distinct red-giant stages
The Deaths of Stars 1 Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come from? 3. What is a planetary nebula,
The Deaths of Stars 1
The Deaths of Stars 1 Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come from? 3. What is a planetary nebula,
Brock University. Test 1, January, 2015 Number of pages: 9 Course: ASTR 1P02 Number of Students: 500 Date of Examination: January 29, 2015
Brock University Test 1, January, 2015 Number of pages: 9 Course: ASTR 1P02 Number of Students: 500 Date of Examination: January 29, 2015 Number of hours: 50 min Time of Examination: 18:00 15:50 Instructor:
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
Stellar Evolution. Stars are chemical factories The Earth and all life on the Earth are made of elements forged in stars
Lecture 11 Stellar Evolution Stars are chemical factories The Earth and all life on the Earth are made of elements forged in stars A Spiral Galaxy (Milky Way Type) 120,000 ly A few hundred billion stars
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!
Stellar Evolution: The Deaths of Stars. Guiding Questions. Pathways of Stellar Evolution. Chapter Twenty-Two
Stellar Evolution: The Deaths of Stars Chapter Twenty-Two Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come
Guiding Questions. The Deaths of Stars. Pathways of Stellar Evolution GOOD TO KNOW. Low-mass stars go through two distinct red-giant stages
The Deaths of Stars Guiding Questions 1. What kinds of nuclear reactions occur within a star like the Sun as it ages? 2. Where did the carbon atoms in our bodies come from? 3. What is a planetary nebula,
Probing the Cosmos with light and gravity: multimessenger astronomy in the gravitational wave era
Utah State University DigitalCommons@USU Colloquia and Seminars Astrophysics 9-7-2011 Probing the Cosmos with light and gravity: multimessenger astronomy in the gravitational wave era Shane L. Larson Utah
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
Astronomy Ch. 21 Stellar Explosions. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Name: Period: Date: Astronomy Ch. 21 Stellar Explosions MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) A surface explosion on a white dwarf, caused
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),
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 &
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
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
Stellar-Mass Black Holes and Pulsars
Stellar-Mass Black Holes and Pulsars Anthony Rushton Work group 2 leader (ESO ALMA fellow) 2010-06-24 Overview of Work Group 2 Stellar-mass black holes and pulsars Two work group leaders: Anthony Rushton
Part two of a year-long introduction to astrophysics:
ASTR 3830 Astrophysics 2 - Galactic and Extragalactic Phil Armitage office: JILA tower A909 email: pja@jilau1.colorado.edu Spitzer Space telescope image of M81 Part two of a year-long introduction to astrophysics:
Learning Objectives: Chapter 13, Part 1: Lower Main Sequence Stars. AST 2010: Chapter 13. AST 2010 Descriptive Astronomy
Chapter 13, Part 1: Lower Main Sequence Stars Define red dwarf, and describe the internal dynamics and later evolution of these low-mass stars. Appreciate the time scale of late-stage stellar evolution
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
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,
Binary Black Holes, Gravitational Waves, & Numerical Relativity Part 1
1 Binary Black Holes, Gravitational Waves, & Numerical Relativity Part 1 Joan Centrella Chief, Gravitational Astrophysics Laboratory NASA/GSFC Summer School on Nuclear and Particle Astrophysics: Connecting
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)
For instance, due to the solar wind, the Sun will lose about 0.1% of its mass over its main sequence existence.
7/7 For instance, due to the solar wind, the Sun will lose about 0.1% of its mass over its main sequence existence. Once a star evolves off the main sequence, its mass changes more drastically. Some stars
Lecture 9: Supernovae
Lecture 9: Supernovae Senior Astrophysics 2018-03-28 Senior Astrophysics Lecture 9: Supernovae 2018-03-28 1 / 35 Outline 1 Core collapse 2 Supernova 3 SN 1987A 4 Next lecture Senior Astrophysics Lecture
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
A1199 Are We Alone? " The Search for Life in the Universe
! A1199 Are We Alone? " The Search for Life in the Universe Instructor: Shami Chatterjee! Summer 2018 Web Page: http://www.astro.cornell.edu/academics/courses/astro1199/! HW2 now posted...! So far: Cosmology,
Physics 5K Lecture 5 - Friday May 4, Atoms. Joel Primack Physics Department UCSC. Friday, May 4, 12
Physics 5K Lecture 5 - Friday May 4, 2012 Atoms Joel Primack Physics Department UCSC Giancoli The Electromagnetic Spectrum Brief History of Atomic Theory 1904 Joseph J. Thomson s "Plum Pudding" model
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
Gravity. Newtonian gravity: F = G M1 M2/r 2
Gravity Einstein s General theory of relativity : Gravity is a manifestation of curvature of 4- dimensional (3 space + 1 time) space-time produced by matter (metric equation? g μν = η μν ) If the curvature
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
Instructions. Students will underline the portions of the PowerPoint that are underlined.
STARS Instructions Students will underline the portions of the PowerPoint that are underlined. Nuclear Furnace 1. A star is like a gigantic nuclear furnace. 2. The nuclear reactions inside convert hydrogen
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
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
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
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
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