Boris Gänsicke. Binary Stars. STFC Summer School (a small selection)
|
|
|
- Egbert O’Connor’
- 5 years ago
- Views:
Transcription
1 Boris Gänsicke Binar Stars (a small selection) STFC Summer School 2008
2 Wh do we care about binar stars? - 50% of all stars are in binaries - (some kind of) white dwarf binaries are SNIa progenitors - binar neutron star mergers make short -ra bursts - Low-mass X-ra binaries, black hole binaries, milli-second pulsars, cataclsmic variables, smbiotic stars All compact binaries share some interesting phsics - go through at least one phase - lose orbital angular momentum
3 Common envelope evolution Willems & Kolb (2004)
4 Common envelope hdrodnamical models courtes of E. Sandquist
5 Planetar nebula: spherical & bipolar
6 Common envelope evolution angular momentum loss Willems & Kolb (2004)
7 Gravitational wave radiation (Einsteins quadrupole eqation): time scale for orbital deca:
8 Examples WD Donor tpical cataclsmic variable WD-WD merger 2R
9 time scale for orbital deca: Stellar magnetic wind braking
10 Equipotential contours in a binar star Edouard Roche ( ) Joseph Lagrange ( )
11 Jupiter-Sun: Trojan asteroids in L4&5
12 Binar star configurations and mass transfer Detached Semidetached: mass transfer via Roche lobe overflow Contact
13 Gravitational (potential) energ surface gravit: M,R m grav. force: work: total work / potential energ:
14 Accretion: a gravitational power plant potential energ: kinetic energ: thermal energ: radiation:
15 Examples: White dwarf
16 Example: Neutron star
17 Example: Stellar black hole
18 Example: Active galactic nucleus (AGN)
19 Accretion onto compact objects
20 Binar star zoolog M 1 >M 2, M 1 evolves first. Wide binar? No interaction, evolve as single stars. wind accretion WD+WD P~hours - das High mass X-ra binar (HMXB), P~das - months RLOF,wind red giant mass donor smbiotic stars P~weeks - ears detached WD/NS/BH + MS binar P~das - ears WD+MS binar cataclsmic variable P~80min 1da SNIa RLOF NS/BH+MS binar low mass X-ra binar (LMXB), P~1h - das WD+BD binar NS+NS SNIa -ra bursts (GRB)
21 Binar star zoolog M 1 >M 2, M 1 evolves first. Wide binar? No interaction, evolve as single stars. Sokoloski et al., 2006, Nature 442, 276 recurrent nova RS Ophiuchi wind accretion WD+WD P~hours - das High mass X-ra binar (HMXB), P~das - months RLOF,wind red giant mass donor smbiotic stars P~weeks - ears detached WD/NS/BH + MS binar P~das - ears WD+MS binar cataclsmic variable P~80min 1da SNIa RLOF NS/BH+MS binar low mass X-ra binar (LMXB), P~1h - das WD+BD binar NS+NS SNIa -ra bursts (GRB)
22 CK Vul = Nova Vulpeculae 1670 Hevelius (1670, Phil. Trans. Ro. Soc. 5, No. 65, 2087)
23 Classical novae: explosive hdrogen shell burning CO/ONeMg H accretion builds up an envelope of hdrogen T & P at the base of the envelope increase Eventuall, conditions for p-p fusion are met If the base of the envelope is degenerate, At, CNO burning takes over, are radioactive ( - ) with h.l. times of ~ s deposit large amounts of energ in the envelope Eventuall, degenerac is lifted, and the nova shell expands Enrichment in Ne is observed in some nova, suggests dredge-up from the white dwarf core
24 Hdrodnamical simulations: 14O concentration 30sec 80sec 1800km x 1000km 100sec 200sec
25 Tpical classical novae V1500 Cg, Nova 1975 das
26 Does the white dwarf grow in mass?
27 Binar star zoolog M1>M2, M1 evolves first. Wide binar? No interaction, evolve as single stars. wind accretion WD+WD P~hours - das High mass X-ra binar (HMXB), P~das - months RLOF,wind red giant mass donor smbiotic stars P~weeks - ears detached WD/NS/BH + MS binar P~das - ears RLOF WD+MS binar NS/BH+MS binar cataclsmic variable low mass X-ra binar P~80min 1da (LMXB), P~1h - das NS+NS SNIa SNIa WD+BD binar -ra bursts (GRB)
28 Binar star zoolog M1>M2, M1 evolves first. Wide binar? No interaction, evolve as single stars. wind accretion WD+WD P~hours - das High mass X-ra binar (HMXB), P~das - months RLOF,wind red giant mass donor smbiotic stars P~weeks - ears detached WD/NS/BH + MS binar P~das - ears RLOF WD+MS binar NS/BH+MS binar cataclsmic variable low mass X-ra binar SNIa Maxted et al., 2006, Nature 442, 543 P~80min 1da (LMXB), P~1h - das NS+NS SNIa WD+BD binar -ra bursts (GRB)
29 Mass distribution of MS-MS binaries BD desert Grether & Lineweaver (2006, ApJ ) Maxted et al. (2006, Nature 442, 543)
30 Binar star zoolog M1>M2, M1 evolves first. Wide binar? No interaction, evolve as single stars. wind accretion WD+WD P~hours - das High mass X-ra binar (HMXB), P~das - months RLOF,wind red giant mass donor smbiotic stars P~weeks - ears detached WD/NS/BH + MS binar P~das - ears RLOF WD+MS binar NS/BH+MS binar cataclsmic variable low mass X-ra binar P~80min 1da (LMXB), P~1h - das NS+NS SNIa SNIa WD+BD binar -ra bursts (GRB)
31 Binar star zoolog M1>M2, M1 evolves first. Wide binar? No interaction, evolve as single stars. wind accretion WD+WD P~hours - das RLOF,wind red giant mass donor smbiotic stars P~weeks - ears detached WD/NS/BH + MS binar P~das - ears High mass X-ra binar (HMXB), P~das - months intermediate polar RLOF NS/BH+MS binar WD+MS binar cataclsmic variable low mass X-ra binar (LMXB), P~1h - das P~80min 1da NS+NS SNIa SNIa WD+BD binar -ra bursts (GRB)
32 Cataclsmic Variables AAVSO data of the dwarf nova U Geminorum
33 SS Cgni: observations in 103 ears
34 Accretion disc instabilit courtes of M. Garlick
35 September 5, 2007 what a da! BTG 19:01UT
36 September 5, 2007 what a da! 19:11UT
37 September 5, 2007 what a da! 20:07UT
38 Rise to the Kroneri observator b x er t h rig
39 Formation of an accretion disc transport of M inwards L outwards (the other half: boundar laer disc and star between )
40 The Ansatz for the viscosit 4th most-cited astrophsics paper
41 Accretion discs can not be spatiall resolved courtes of M. Garlick
42 Accretion discs can not be spatiall resolved courtes of M. Garlick
43 Making the invisible visible I: NMR & CT imaging
44 Making the invisible visible II: Doppler tomograph
45 bright spots in Doppler maps GP Comae
46 The components of a binar star in a Doppler map
47 Time-resolved Doppler maps (D. Steeghs)
48 Binar star zoolog M1>M2, M1 evolves first. Wide binar? No interaction, evolve as single stars. wind accretion WD+WD P~hours - das High mass X-ra binar (HMXB), P~das - months RLOF,wind red giant mass donor smbiotic stars P~weeks - ears detached WD/NS/BH + MS binar P~das - ears RLOF WD+MS binar NS/BH+MS binar cataclsmic variable low mass X-ra binar P~80min 1da (LMXB), P~1h - das NS+NS SNIa SNIa WD+BD binar -ra bursts (GRB)
49 Binar star zoolog spectral No interaction, evolve as single stars. tpe ~ G0-G2 M1>M2, M1 evolves first. Wide binar? wind accretion Tcho Brahe s SN1572 Ruiz-Lapuente et al. 2004, Nature 431, 1069 High mass X-ra binar (HMXB), P~das - months RLOF,wind red giant mass donor smbiotic stars P~weeks - ears detached WD/NS/BH + MS binar P~das - ears RLOF WD+MS binar NS/BH+MS binar cataclsmic variable low mass X-ra binar P~80min 1da (LMXB), P~1h - das NS+NS SNIa SNIa WD+BD binar -ra bursts (GRB)
50 Mass-radius relation of compact stars white dwarfs: Chandrasekhar 1935
51 SNIa: the last seconds of an accreting white dwarf approaching the Chandrasehkar limit, WD rapidl shrinks ion gas (C/O) is not degenerate, hence heats up (P=NkT) C/O burning starts in the core, producing heavier elements up to iron nuclear flame propagates outwards: subsonic (deflagration) or supersonic (detonation)? Not well known
52 movie time
53 The first progenitor detection of a SNIa? SN2007on in NGC1404 pre-explosion Chandra X-ra image pre-explosion HST optical image post-explosion Swift optical image Voss & Nelemans (2008, Nature 451, 802)
54 Binar star zoolog M1>M2, M1 evolves first. Wide binar? No interaction, evolve as single stars. wind accretion WD+WD P~hours - das High mass X-ra binar (HMXB), P~das - months RLOF,wind red giant mass donor smbiotic stars P~weeks - ears detached WD/NS/BH + MS binar P~das - ears RLOF WD+MS binar NS/BH+MS binar cataclsmic variable low mass X-ra binar P~80min 1da (LMXB), P~1h - das NS+NS SNIa SNIa WD+BD binar -ra bursts (GRB)
55 Binar star zoolog Porb=685sec M1>M2, M1 evolves first. Wide binar? No interaction, evolve as single stars. wind accretion WD+WD P~hours - das High mass X-ra binar (HMXB), P~das - months RLOF,wind red giant mass donor smbiotic stars P~weeks - ears detached WD/NS/BH + MS binar P~das - ears RLOF WD+MS binar NS/BH+MS binar cataclsmic variable low mass X-ra binar P~80min 1da (LMXB), P~1h - das NS+NS SNIa SNIa WD+BD binar -ra bursts (GRB)
56 The mass function companion:spectral tpe ~K mass function Kepler III
57 Weighing the X-ra nova A = V616 Mon
58 Weighing the X-ra nova A = V616 Mon companion:spectral tpe ~K Rotational velocit of a Roche-lobe filling star:
59 Weighing the X-ra nova A = V616 Mon ellipsoidal modulation
60 Black hole binaries Mʘ 10-18Mʘ Mʘ Mʘ Mʘ Mʘ Mʘ Mʘ Mʘ Mʘ Mʘ Mʘ Mʘ??Mʘ Mʘ Mʘ
61 Binar star zoolog M1>M2, M1 evolves first. Wide binar? No interaction, evolve as single stars. wind accretion WD+WD P~hours - das High mass X-ra binar (HMXB), P~das - months RLOF,wind red giant mass donor smbiotic stars P~weeks - ears detached WD/NS/BH + MS binar P~das - ears RLOF WD+MS binar NS/BH+MS binar cataclsmic variable low mass X-ra binar P~80min 1da (LMXB), P~1h - das NS+NS SNIa SNIa WD+BD binar -ra bursts (GRB)
62 Binar star zoolog M1>M2, M1 evolves first. Wide binar? No interaction, evolve as single stars. wind accretion WD+WD P~hours - das High mass X-ra binar (HMXB), P~das - months RLOF,wind red giant mass donor smbiotic stars P~weeks - ears detached WD/NS/BH + MS binar P~das - ears RLOF WD+MS binar NS/BH+MS binar cataclsmic variable low mass X-ra binar P~80min 1da (LMXB), P~1h - das NS+NS SNIa SNIa WD+BD binar -ra bursts (GRB)
63 Binar star zoolog M1>M2, M1 evolves first. Wide binar? No interaction, evolve as single stars. wind accretion WD+WD P~hours - das High mass X-ra binar (HMXB), P~das - months RLOF,wind red giant mass donor smbiotic stars P~weeks - ears detached WD/NS/BH + MS binar P~das - ears RLOF WD+MS binar NS/BH+MS binar cataclsmic variable low mass X-ra binar P~80min 1da (LMXB), P~1h - das NS+NS SNIa SNIa WD+BD binar -ra bursts (GRB)
64 22.5min in the life of PSR uncorrected for binar orbit corrected for binar orbit
65 The binar pulsar PSR pulse period varies over the binar orbit due to the Doppler effect
66 The binar pulsar PSR gravitational wave radiation GR confirmed to better than 1% 1993: Nobel prize for Hulse & Talor
67 Relativistic neutron star binaries NS-NS NS-WD
68 Binar star zoolog M1>M2, M1 evolves first. Wide binar? No interaction, evolve as single stars. wind accretion WD+WD P~hours - das High mass X-ra binar (HMXB), P~das - months RLOF,wind red giant mass donor smbiotic stars P~weeks - ears detached WD/NS/BH + MS binar P~das - ears RLOF WD+MS binar NS/BH+MS binar cataclsmic variable low mass X-ra binar P~80min 1da (LMXB), P~1h - das NS+NS SNIa SNIa WD+BD binar -ra bursts (GRB)
69 Binar star zoolog M1>M2, M1 evolves first. Wide binar? No interaction, evolve as single stars. wind accretion WD+WD P~hours - das High mass X-ra binar (HMXB), P~das - months RLOF,wind red giant mass donor smbiotic stars P~weeks - ears detached WD/NS/BH + MS binar P~das - ears RLOF WD+MS binar NS/BH+MS binar cataclsmic variable low mass X-ra binar P~80min 1da (LMXB), P~1h - das NS+NS SNIa SNIa WD+BD binar -ra bursts (GRB)
Boris Gänsicke. Type Ia supernovae and their progenitors
Boris Gänsicke Type Ia supernovae and their progenitors November 1572, in Cassiopeia: a nova a new star V~-4 Tycho Brahe: De nova et nullius aevi memoria prius visa stella (1602) October 9, 1604, in Ophiuchus
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
Lecture 13: Binary evolution
Lecture 13: Binary evolution Senior Astrophysics 2017-04-12 Senior Astrophysics Lecture 13: Binary evolution 2017-04-12 1 / 37 Outline 1 Conservative mass transfer 2 Non-conservative mass transfer 3 Cataclysmic
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$
Unstable Mass Transfer
Unstable Mass Transfer When the mass ratios are large, or when the donor star has a deep convective layer (so R M-1/3), mass loss will occur on a dynamical timescale. The result will be common envelope
The Evolution of Close Binaries
The Evolution of Close Binaries Philipp Podsiadlowski (Oxford) The case of RS Ophiuchi as a test of binary stellar evolution as a potential Type Ia supernova (SN Ia) progenitor I. Testing Binary Evolution:
Dr. Reed L. Riddle. Close binaries, stellar interactions and novae. Guest lecture Astronomy 20 November 2, 2004
Dr. Reed L. Riddle Close binaries, stellar interactions and novae Guest lecture Astronomy 20 November 2, 2004 Gravitational Tides Look at the forces acting on one body orbiting another - more pull on closer
Accretion in Binaries
Accretion in Binaries Two paths for accretion Roche-lobe overflow Wind-fed accretion Classes of X-ray binaries Low-mass (BH and NS) High-mass (BH and NS) X-ray pulsars (NS) Be/X-ray binaries (NS) Roche
Dr G. I. Ogilvie Lent Term 2005 INTRODUCTION
Accretion Discs Mathematical Tripos, Part III Dr G. I. Ogilvie Lent Term 2005 INTRODUCTION 0.1. Accretion If a particle of mass m falls from infinity and comes to rest on the surface of a star of mass
7. BINARY STARS (ZG: 12; CO: 7, 17)
7. BINARY STARS (ZG: 12; CO: 7, 17) most stars are members of binary systems or multiple systems (triples, quadruples, quintuplets,...) orbital period distribution: P orb = 11 min to 10 6 yr the majority
The Evolution of Binary-Star Systems
The Evolution of Binary-Star Systems If the stars in a binary-star system are relatively widely separated, their evolution proceeds much as it would have if they were not companions... If they are closer,
Basics, types Evolution. Novae. Spectra (days after eruption) Nova shells (months to years after eruption) Abundances
Basics, types Evolution Novae Spectra (days after eruption) Nova shells (months to years after eruption) Abundances 1 Cataclysmic Variables (CVs) M.S. dwarf or subgiant overflows Roche lobe and transfers
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
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
Names: Team: Team Number:
Astronomy C Michigan Region 8 March 11, 2017 Names: Team: Team Number: Directions 1. There is a separate answer sheet. Answers written elsewhere (e.g. on the test) will not be considered. 2. You may take
Astronomy Ch. 20 Stellar Evolution. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Name: Period: Date: Astronomy Ch. 20 Stellar Evolution MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) A star (no matter what its mass) spends
Astronomy Ch. 20 Stellar Evolution. MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question.
Name: Period: Date: Astronomy Ch. 20 Stellar Evolution MULTIPLE CHOICE. Choose the one alternative that best completes the statement or answers the question. 1) A star (no matter what its mass) spends
Cataclysmic variables
Cataclysmic variables Sander Bus Kapteyn Astronomical Institute Groningen October 6, 2011 Overview Types of cataclysmic stars How to form a cataclysmic variable X-ray production Variation in outburst lightcurve,
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
Distant Type Ia supernova Refsdal gravitationally lensed, appears multiple places and times.
Friday, March 6, 2015 Reading for Exam 3: Chapter 6, end of Section 6 (binary evolution), Section 6.7 (radioactive decay), Chapter 7 (SN 1987A) Background in Chapters 3, 4, 5. Background: Sections 3.1,
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
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
Gravitational Waves from Compact Object Binaries
Gravitational Waves from Compact Object Binaries Ashley J. Ruiter New Mexico State University / Center for Astrophysics Graduate Student / Pre-doctoral Fellow Dr. Chris Belczynski (PhD Advisor) Los Alamos
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
Einführung in die Astronomie II
Einführung in die Astronomie II Teil 10 Peter Hauschildt yeti@hs.uni-hamburg.de Hamburger Sternwarte Gojenbergsweg 112 21029 Hamburg 15. Juni 2017 1 / 47 Overview part 10 Death of stars AGB stars PNe SNe
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
Distribution of X-ray binary stars in the Galaxy (RXTE) High-Energy Astrophysics Lecture 8: Accretion and jets in binary stars
High-Energy Astrophysics Lecture 8: Accretion and jets in binary stars Distribution of X-ray binary stars in the Galaxy (RXTE) Robert Laing Primary Compact accreting binary systems Compact star WD NS BH
Binary stars, their role as determining the specific properties of stars, cluster history and in novae creation
Binary stars, their role as determining the specific properties of stars, cluster history and in novae creation By Emilio GARCIA 13/03/2007 Uppsala University Course:1FA223 - Report code:63061 I Introduction
6 th lecture of Compact Object and Accretion, Master Programme at Leiden Observatory
6 th lecture of Compact Object and Accretion, Master Programme at Leiden Observatory Accretion 1st class study material: Chapter 1 & 4, accretion power in astrophysics these slides at http://home.strw.leidenuniv.nl/~emr/coa/
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
Astronomy in the news? Government shut down. No astronomy picture of the day
Wednesday, October 2, 2013 Exam 2 Friday. Review sheet posted. Review session Tomorrow, 5 6 PM, WRW 102 Reading: Sections 6.1 (Type Ib/c), 6.4, 6.5 (but not detail on polarization), 6.6, Betelgeuse, Section
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
The Origin of Type Ia Supernovae
The Origin of Type Ia Supernovae Gijs Nelemans Radboud University Nijmegen with Rasmus Voss, Mikkel Nielsel, Silvia Toonen, Madelon Bours, Carsten Dominik Outline Introduction: supernovae Relevance Type
Relativistic Astrophysics Neutron Stars, Black Holes & Grav. W. ... A brief description of the course
Relativistic Astrophysics Neutron Stars, Black Holes & Grav. Waves... A brief description of the course May 2, 2009 Structure of the Course Introduction to General Theory of Relativity (2-3 weeks) Gravitational
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
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
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)
Outline. Stellar Explosions. Novae. Death of a High-Mass Star. Binding Energy per nucleon. Nova V838Mon with Hubble, May Dec 2002
Outline Novae (detonations on the surface of a star) Supernovae (detonations of a star) The Mystery of Gamma Ray Bursts (GRBs) Sifting through afterglows for clues! Stellar Explosions Novae Nova V838Mon
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
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
Rocket experiments. Sco X-1. Giacconi et al. 1962
X-ray binaries Rocket experiments. Sco X-1 Giacconi et al. 1962 Binaries are important and different! Wealth of observational manifestations: Visual binaries orbits, masses Close binaries effects of mass
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?
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
Evolution and Final Fates of Accreting White Dwarfs. Ken Nomoto (Kavli IPMU / U. Tokyo)
Evolution and Final Fates of Accreting White Dwarfs Ken Nomoto (Kavli IPMU / U. Tokyo) AD 1572 Korean & Chinese Record Guest Star as bright as Venus (Sonjo Sujong Sillok: Korea) AD 1572 Tycho Brahe s Supernova
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
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
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
The Algol Mystery. Binary Evolution Novae, Supernovae, and X-ray Sources. Algol. Mass Transfer in Binaries
The Algol Mystery Binary Evolution Novae, Supernovae, and X-ray Sources http://apod.nasa.gov/apod/ Algol is a double-lined eclipsing binary system with a period of about 3 days (very short). The two stars
School and Conference on Analytical and Computational Astrophysics November, Introduction to Accretion Phenomena in Astrophysics
2292-2 School and Conference on Analytical and Computational Astrophysics 14-25 November, 2011 Introduction to Accretion Phenomena in Astrophysics Andria Rogava Georgian National Astrophysical Laboratory,
Nuclear Astrophysics
Nuclear Astrophysics IV: Novae, x-ray bursts and thermonuclear supernovae Karlheinz Langanke GSI & TU Darmstadt Aarhus, October 6-10, 2008 Karlheinz Langanke ( GSI & TU Darmstadt) Nuclear Astrophysics
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
X-ray observations of X-ray binaries and AGN
X-ray observations of X-ray binaries and AGN Tomaso M. Be!oni (INAF - Osservatorio Astronomico di Brera) (Visiting Professor, Univ. of Southampton) OUTLINE Lecture I: Accretion onto compact objects, X-ray
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
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
Binary Evolution Novae, Supernovae, and X-ray Sources
Binary Evolution Novae, Supernovae, and X-ray Sources The Algol Mystery Algol is a double-lined eclipsing binary system with a period of about 3 days (very short). The two stars are: Star A: B8, 3.4M o
The Deaths of Stars. The Southern Crab Nebula (He2-104), a planetary nebula (left), and the Crab Nebula (M1; right), a supernova remnant.
The Deaths of Stars The Southern Crab Nebula (He2-104), a planetary nebula (left), and the Crab Nebula (M1; right), a supernova remnant. Once the giant phase of a mediummass star ends, it exhales its outer
Pulsars ASTR2110 Sarazin. Crab Pulsar in X-rays
Pulsars ASTR2110 Sarazin Crab Pulsar in X-rays Test #2 Monday, November 13, 11-11:50 am Ruffner G006 (classroom) Bring pencils, paper, calculator You may not consult the text, your notes, or any other
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
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
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
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,
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
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.
Mass Transfer in Binaries
Mass Transfer in Binaries Philipp Podsiadlowski (Oxford) Understanding the physics of mass transfer is essential for understanding binary evolution Simplest assumption: stable, conservative mass transfer
Millisecond X-ray pulsars: 10 years of progress. Maurizio Falanga
Millisecond X-ray pulsars: 10 years of progress Maurizio Falanga History I Radio Astronomy in the 30 s-60 s Karl Jansky 1933 3C273 Discovery (1961-63) Quasi-Stellar Radio Sources as the most energetic
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
The structure and evolution of stars. Learning Outcomes
The structure and evolution of stars Lecture14: Type Ia Supernovae The Extravagant Universe By R. Kirshner 1 Learning Outcomes In these final two lectures the student will learn about the following issues:
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
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
Supernova events and neutron stars
Supernova events and neutron stars So far, we have followed stellar evolution up to the formation of a C-rich core. For massive stars ( M initial > 8 M Sun ), the contracting He core proceeds smoothly
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
Quasars, Pulsars, Gamma- Ray Bursts! Oh, my! Collapsars, magnetars, X- ray pulsars, γ-ray pulsars, millisecond radio pulsars...
Quasars, Pulsars, Gamma- Ray Bursts! Oh, my! Collapsars, magnetars, X- ray pulsars, γ-ray pulsars, millisecond radio pulsars... Giacconi et al. (1962) Rocket carried 3 Geiger counters to 225km - one counter
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
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
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
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
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.
Five and a half roads to from a millisecond pulsar. Thomas Tauris AIfA, University of Bonn Max-Planck-Institut für Radioastronomie, Bonn
Five and a half roads to from a millisecond pulsar Thomas Tauris AIfA, University of Bonn Max-Planck-Institut für Radioastronomie, Bonn Evolution of Compact Binaries, ESO Chile, March 6-11, 2011 Millisecond
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 ~
Stars and their properties: (Chapters 11 and 12)
Stars and their properties: (Chapters 11 and 12) To classify stars we determine the following properties for stars: 1. Distance : Needed to determine how much energy stars produce and radiate away by using
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
3/13/18. Things to do. Synchrotron Radiation. Today on Stellar Explosions
ASTR 1040: Stars & Galaxies Prof. Juri Toomre TAs: Peri Johnson, Ryan Horton Lecture 17 Tues 13 Mar 2018 zeus.colorado.edu/astr1040-toomre Ring Nebula Today on Stellar Explosions Revisit Pulsars spinning
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
THE 82ND ARTHUR H. COMPTON LECTURE SERIES
THE 82ND ARTHUR H. COMPTON LECTURE SERIES by Dr. Manos Chatzopoulos Enrico Fermi Postdoctoral Fellow FLASH Center for Computational Science Department of Astronomy & Astrophysics University of Chicago
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
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
Rob Izzard. February 21, University of Utrecht. Binary Star Nucleosynthesis. Nucleosynthesis. Single Star Evolution. Binary Star.
University of Utrecht February 21, 2006 Contents Mechanisms Proton capture: H He via pp-chain, CNO, NeNa, MgAl The Sun and most stars Alpha capture: He C, C O, O Ne... Fe Evolved stars C-burning: C + C
White dwarf populations. Gijs Nelemans Radboud University Nijmegen
White dwarf populations Gijs Nelemans Radboud University Nijmegen Outline Introduction: Population synthesis Basic ingredients Observational inputs White dwarf populations Different types and mergers WD
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
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
Supernovae. Supernova basics Supernova types Light Curves SN Spectra after explosion Supernova Remnants (SNRs) Collisional Ionization
Supernovae Supernova basics Supernova types Light Curves SN Spectra after explosion Supernova Remnants (SNRs) Collisional Ionization 1 Supernova Basics Supernova (SN) explosions in our Galaxy and others
Chapter 21 Stellar Explosions
Chapter 21 Stellar Explosions Units of Chapter 21 21.1 XXLife after Death for White Dwarfs (not on exam) 21.2 The End of a High-Mass Star 21.3 Supernovae Supernova 1987A The Crab Nebula in Motion 21.4
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
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
CATACLYSMIC VARIABLES. AND THE TYPE Ia PROGENITOR PROBLEM PROGENITOR PROBLEM
CATACLYSMIC VARIABLES AND THE TYPE Ia PROGENITOR PROBLEM PROGENITOR PROBLEM Lorne Nelson SNOVAE07 Feb. 23, 2007 Cataclysmic Variables CVs are characterized by a low-mass star/bd (donor) losing mass to
SN1987A before(right) and during the explosion. Supernova Explosion. Qingling Ni
SN1987A before(right) and during the explosion Supernova Explosion Qingling Ni Overview Core-Collapse supernova (including Type II supernova) -Mechanism: collapse+rebound Type Ia supernova -Mechanism:
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
Announcement: Quiz Friday, Oct 31
Announcement: Quiz Friday, Oct 31 What is the difference between the giant, horizontal, and asymptotic-giant branches? What is the Helium flash? Why can t high-mass stars support themselves in hydrostatic
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
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,