The spin of the second-born Black hole in coalescing double BH b

Size: px
Start display at page:

Download "The spin of the second-born Black hole in coalescing double BH b"

Transcription

1 The spin of the second-born Black hole in coalescing double BH binaries Ying Qin Tassos Fragos, Georges Meynet Geneva Observatory, University of Geneva FOE, June 5-8, 2017

2 Background: Why the spin of the BH is important? Spin of the stellar-mass BH: a = c ~ J GM 2, 0 6 a Cover Half information of the BH 2 Related to the formation of long Gamma-ray Bursts 3 Distinguish the double BH formation channels

3 Background: Spin measurements from AdLIGO team

4 Progenitor of the GW (Belczynski et al. Nature 534,512B, 2016)

5 The spin of the first BH Metallicity, Mass, Magnetic field (Taylor-Spruit mechanism), init. MESA

6 The spin of the first BH Metallicity, Mass, Magnetic field (Taylor-Spruit mechanism), init. MESA a ) Negligible!

7 Observation from AdLIGO Constraint on the spin of the second-born BH from e

8 Progenitor of the GW (Belczynski et al. Nature 534,512B, 2016)

9 The spin of the second-born BH Angular momentum evolution of the He star Stellar wind () Tides He star: Dynamical tides (Radiative envelope + convective core)

10 The spin of the second-born BH Angular momentum evolution of the He star Stellar wind () Tides He star: Dynamical tides (Radiative envelope + convective core) Timescale of the synchronization (Hut 1981; Zahn 1975,1977) 1 T sync = 1 n d dt =3 (GM R 3 )1/2 q 2 (1 + q) 5/6 MR2 I E 2 ( R a )17/2

11 The spin of the second-born BH Angular momentum evolution of the He star Stellar wind () Tides He star: Dynamical tides (Radiative envelope + convective core) Timescale of the synchronization (Hut 1981; Zahn 1975,1977) 1 T sync = 1 n d dt =3 (GM R 3 )1/2 q 2 (1 + q) 5/6 MR2 I E 2 ( R a )17/2 E 2 = ( M M )2.84 (Hurley et al. 2002) E 2 = ( Rconv R )8 (Yoon et al. 2010)

12 Tidal coe cient E 2 (Zahn 1977) Solution of the E 2 3 8/3 ( (4/3)) 2 3 f R E n = (2n +1)[n(n +1)] 4/3 M [ R ( g s gb x 2 )0 f ] 1/3 2 H n Z 1 xf H n = X (x f )Y (1) 0 [Y 00 n(n +1)Y x 2 ]Xdx Y 00 6(1 X 00 0 ) Y 0 x X 0 n(n +1) x 2 X =0 [n(n +1) 12(1 )] Y x 2 =0

13 Tidal coe cient E 2 (Zahn 1977) Solution of the E 2 3 8/3 ( (4/3)) 2 3 f R E n = (2n +1)[n(n +1)] 4/3 M [ R ( g s gb x 2 )0 f ] 1/3 2 H n Fitting results at di erent metalliciy 1 Hrichstars Z 1 xf H n = X (x f )Y (1) 0 [Y 00 n(n +1)Y x 2 ]Xdx 2 He stars E 2 = ( R conv R )7.46 Y 00 6(1 X 00 0 ) Y 0 x X 0 n(n +1) x 2 X =0 [n(n +1) 12(1 )] Y x 2 =0 E 2 = ( R conv R )8.14

14 Tidal e ciency

15 Tidal e ciency M He [M ]: 4,8,..,50 P orb [days]: ) P orb <2

16 He star (1% Z ) + compact objects: Spin on the second-born BH

17 He star (Z ) + compact objects: Spin on the second-born BH

18 He star (1% Z ) + compact objects: Merger timescale

19 He star (1% Z ) + compact objects: Spin vs Merger timescale Lower spin of the second-born BH () Longer timescale of the merger

20 SUMMARY

21 SUMMARY 1 The spin of the first BH is negligible

22 SUMMARY 1 The spin of the first BH is negligible 2 Tides become important only for close binaries (P orb <2days)

23 SUMMARY 1 The spin of the first BH is negligible 2 Tides become important only for close binaries (P orb <2days) 3 The spin of the second-born BH: 0! 1

24 SUMMARY 1 The spin of the first BH is negligible 2 Tides become important only for close binaries (P orb <2days) 3 The spin of the second-born BH: 0! 1 4 Anti-correlation between the timescale of the merger and the spin of the second-born BH

25 SUMMARY 1 The spin of the first BH is negligible 2 Tides become important only for close binaries (P orb <2days) 3 The spin of the second-born BH: 0! 1 4 Anti-correlation between the timescale of the merger and the spin of the second-born BH Thanks for your attention!!!

FORMATION AND EVOLUTION OF COMPACT BINARY SYSTEMS

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

More information

Stellar models for a wide range of initial chemical compositions until helium burning

Stellar models for a wide range of initial chemical compositions until helium burning ASTRONOMY & ASTROPHYSICS NOVEMBER I 1997, PAGE 439 SUPPLEMENT SERIES Astron. Astrophys. Suppl. Ser. 125, 439-443 (1997) Stellar models for a wide range of initial chemical compositions until helium burning

More information

Massive Stellar Black Hole Binaries and Gravitational Waves

Massive Stellar Black Hole Binaries and Gravitational Waves BH-BH binaries: modeling Massive Stellar Black Hole Binaries and Gravitational Waves Chris Belczynski1 Tomek Bulik1 Daniel Holz Richard O Shaughnessy Wojciech Gladysz1 and Grzegorz Wiktorowicz1 1 Astronomical

More information

A new route towards merging massive black holes

A new route towards merging massive black holes A new route towards merging massive black holes Pablo Marchant 1, Norbert Langer 1, Philipp Podsiadlowski 2,1, Thomas Tauris 1,3, Takashi Moriya 1, Lise de Buisson 2, Selma de Mink 4 and Ilya Mandel 5

More information

Binary black holes: formation scenarios and merger rates

Binary black holes: formation scenarios and merger rates Binary black holes: formation scenarios and merger rates Tomasz Bulik Astronomical Observatory University of Warsaw 1 Gravitational waves: physical background Spacetime oscillations Gravitational waves

More information

Open problems in compact object dynamics

Open problems in compact object dynamics Open problems in compact object dynamics Melvyn B. Davies Department of Astronomy and Theoretical Physics Lund University www.astro.lu.se Key ideas and open questions in compact object dynamics Melvyn

More information

What have we learned from the detection of gravitational waves? Hyung Mok Lee Seoul National University

What have we learned from the detection of gravitational waves? Hyung Mok Lee Seoul National University What have we learned from the detection of gravitational waves? Hyung Mok Lee Seoul National University Outline Summary of 1st and 2nd Observing Runs Characteristics of detected sources Astrophysical Implications

More information

Gravitational Waves from Compact Object Binaries

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

More information

Pulsars ASTR2110 Sarazin. Crab Pulsar in X-rays

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

More information

Rotation in White Dwarfs: Stellar Evolution Models

Rotation in White Dwarfs: Stellar Evolution Models 15 th European Workshop on White Dwarfs ASP Conference Series, Vol. 372, 2007 R. Napiwotzki and M. R. Burleigh Rotation in White Dwarfs: Stellar Evolution Models N. Langer Sterrenkundig Instituut, Utrecht

More information

Pulsations and Magnetic Fields in Massive Stars. Matteo Cantiello KITP Fellow Kavli Institute for Theoretical Physics, UCSB

Pulsations and Magnetic Fields in Massive Stars. Matteo Cantiello KITP Fellow Kavli Institute for Theoretical Physics, UCSB Pulsations and Magnetic Fields in Massive Stars Matteo Cantiello KITP Fellow Kavli Institute for Theoretical Physics, UCSB Massive stars Energy / Momentum in ISM Stellar Winds, SNe Nucleosynthesis Remnants:

More information

Long Gamma Ray Bursts from metal poor/pop III stars. Sung-Chul Yoon (Amsterdam) Norbert Langer (Utrecht) Colin Norman (JHU/STScI)

Long Gamma Ray Bursts from metal poor/pop III stars. Sung-Chul Yoon (Amsterdam) Norbert Langer (Utrecht) Colin Norman (JHU/STScI) Long Gamma Ray Bursts from metal poor/pop III stars Sung-Chul Yoon (Amsterdam) Norbert Langer (Utrecht) Colin Norman (JHU/STScI) The First Stars and Evolution of the Early Universe, Seattle, June 06, 2006

More information

Rocket experiments. Sco X-1. Giacconi et al. 1962

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

More information

Advanced Binary Evolution

Advanced Binary Evolution Massive Stars in Interacting Binaries ASP Conference Series, Vol. 367, 2007 N. St-Louis & A.F.J. Moffat Advanced Binary Evolution N. Langer & J. Petrovic Astronomical Institute, Utrecht University Abstract.

More information

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 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/

More information

Stellar collisions and their products

Stellar collisions and their products Stellar collisions and their products Melvyn B. Davies Department of Astronomy and Theoretical Physics Lund University www.astro.lu.se KEY IDEA #1 Collision rate depends on V. Stellar encounter timescales

More information

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 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

More information

Optical/IR Counterparts of GW Signals (NS-NS and BH-NS mergers)

Optical/IR Counterparts of GW Signals (NS-NS and BH-NS mergers) Optical/IR Counterparts of GW Signals (NS-NS and BH-NS mergers) Chris Belczynski 1,2 1 Warsaw University Observatory 2 University of Texas, Brownsville Theoretical Rate Estimates (MOSTLY NS-NS MERGERS:

More information

Insights into binary evolution from gravitational waves

Insights into binary evolution from gravitational waves Insights into binary evolution from gravitational waves Simon Stevenson simon.stevenson@ligo.org @simon4nine For the COMPAS team Alejandro Vigna-Gomez, Jim Barrett, Coen Nijssell, Christopher Berry, Ilya

More information

arxiv:astro-ph/ v2 5 Aug 1997

arxiv:astro-ph/ v2 5 Aug 1997 Dissipation of a tide in a differentially rotating star Suzanne Talon Observatoire de Paris, Section de Meudon, 92195 Meudon, France and arxiv:astro-ph/9707309v2 5 Aug 1997 Pawan Kumar Institute for Advanced

More information

Dynamics of star clusters containing stellar mass black holes: 1. Introduction to Gravitational Waves

Dynamics of star clusters containing stellar mass black holes: 1. Introduction to Gravitational Waves Dynamics of star clusters containing stellar mass black holes: 1. Introduction to Gravitational Waves July 25, 2017 Bonn Seoul National University Outline What are the gravitational waves? Generation of

More information

Understanding Black Hole

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

More information

Gravitational Waves. Masaru Shibata U. Tokyo

Gravitational Waves. Masaru Shibata U. Tokyo Gravitational Waves Masaru Shibata U. Tokyo 1. Gravitational wave theory briefly 2. Sources of gravitational waves 2A: High frequency (f > 10 Hz) 2B: Low frequency (f < 10 Hz) (talk 2B only in the case

More information

Accretion in Binaries

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

More information

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

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

More information

MIDTERM #2. ASTR 101 General Astronomy: Stars & Galaxies. Can we detect BLACK HOLES? Black Holes in Binaries to the rescue. Black spot in the sky?

MIDTERM #2. ASTR 101 General Astronomy: Stars & Galaxies. Can we detect BLACK HOLES? Black Holes in Binaries to the rescue. Black spot in the sky? ASTR 101 General Astronomy: Stars & Galaxies Can we detect BLACK HOLES? NEXT Friday 04/03: MIDTERM #2 [Image by A. Hamilton] Black spot in the sky? Black Holes in Binaries to the rescue Black Holes in

More information

Learning about Black- Hole Forma5on by Observing Gravita5onal Waves. Michael Kesden (UT Dallas) PPC 2017 Mee5ng Corpus Chris5, TX May 22, 2017

Learning about Black- Hole Forma5on by Observing Gravita5onal Waves. Michael Kesden (UT Dallas) PPC 2017 Mee5ng Corpus Chris5, TX May 22, 2017 Learning about Black- Hole Forma5on by Observing Gravita5onal Waves Michael Kesden (UT Dallas) PPC 2017 Mee5ng Corpus Chris5, TX May 22, 2017 Outline What are gravita5onal waves (GWs) and how do observatories

More information

Possible indirect confirmation of the existence of Pop III massive stars by gravitational wave

Possible indirect confirmation of the existence of Pop III massive stars by gravitational wave doi:10.1093/mnras/stu1022 Possible indirect confirmation of the existence of Pop III massive stars by gravitational wave Tomoya Kinugawa, Kohei Inayoshi, Kenta Hotokezaka, Daisuke Nakauchi and Takashi

More information

Compact Binaries as Gravitational-Wave Sources

Compact Binaries as Gravitational-Wave Sources Compact Binaries as Gravitational-Wave Sources Chunglee Kim Lund Observatory Extreme Astrophysics for All 10 February, 2009 Outline Introduction Double-neutron-star systems = NS-NS binaries Neutron star

More information

7. BINARY STARS (ZG: 12; CO: 7, 17)

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

More information

A Comparative Study of Quark-Gluon Plasma at the Core of a Neutron Star and in the Very Early Universe. Frikkie de Bruyn

A Comparative Study of Quark-Gluon Plasma at the Core of a Neutron Star and in the Very Early Universe. Frikkie de Bruyn A Comparative Study of Quark-Gluon Plasma at the Core of a Neutron Star and in the Very Early Universe By Frikkie de Bruyn Introduction 1 Study of quark-gluon plasma fluid is of mutual Interest to both

More information

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 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

More information

14/11/2018. L Aquila - Multi-messenger studies of NS mergers, GRBs and magnetars. Simone Dall Osso

14/11/2018. L Aquila - Multi-messenger studies of NS mergers, GRBs and magnetars. Simone Dall Osso L Aquila - 14/11/2018 Multi-messenger studies of NS mergers, GRBs and magnetars Simone Dall Osso OUTLINE 1. Overview of GW/EM discoveries since 2015 binary black hole mergers binary neutron star mergers

More information

Neutron Star Mass Distribution in Binaries

Neutron Star Mass Distribution in Binaries A Tribute to Gerry@2013.11.26 Neutron Star Mass Distribution in Binaries Chang-Hwan Lee @ Sabbatical Year@Stony Brook (2013.8~2014.8) 1 2 Gerry s Three Questions The Future The Life The Science 3 20 years

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

Quasi-stars and the Cosmic Evolution of Massive Black Holes

Quasi-stars and the Cosmic Evolution of Massive Black Holes Quasi-stars and the Cosmic Evolution of Massive Black Holes Marta Volonteri and Mitchell C. Begelman 2010 MNRAS 409:1022 David Riethmiller January 26, 2011 Outline Two different methods for MBH formation:

More information

Four ways of doing cosmography with gravitational waves

Four ways of doing cosmography with gravitational waves Four ways of doing cosmography with gravitational waves Chris Van Den Broeck National Institute for Subatomic Physics Amsterdam, The Netherlands StronG BaD Workshop, Oxford, Mississippi, 27 February -

More information

Implications of GW observations for short GRBs

Implications of GW observations for short GRBs Implications of GW observations for short GRBs Resmi Lekshmi Indian Institute of Space Science & Technology Trivandrum What are Gamma Ray Bursts? What are short GRBs? Open Questions : Central engine of

More information

Chapter 6: Stellar Evolution (part 2): Stellar end-products

Chapter 6: Stellar Evolution (part 2): Stellar end-products Chapter 6: Stellar Evolution (part 2): Stellar end-products Final evolution stages of high-mass stars Stellar end-products White dwarfs Neutron stars and black holes Supernovae Core-collapsed SNe Pair-Instability

More information

Gravitational waves (...and GRB central engines...) from neutron star mergers

Gravitational waves (...and GRB central engines...) from neutron star mergers Gravitational waves (...and GRB central engines...) from neutron star mergers Roland Oechslin MPA Garching, SFB/TR 7 Ringberg Workshop, 27.3.2007 In this talk: -Intro: -Overview & Motivation -Neutron star

More information

AGN in hierarchical galaxy formation models

AGN in hierarchical galaxy formation models AGN in hierarchical galaxy formation models Nikos Fanidakis and C.M. Baugh, R.G. Bower, S. Cole, C. Done, C. S. Frenk Physics of Galactic Nuclei, Ringberg Castle, June 18, 2009 Outline Brief introduction

More information

Gamma Ray Bursts. Progress & Prospects. Resmi Lekshmi. Indian Institute of Space Science & Technology Trivandrum

Gamma Ray Bursts. Progress & Prospects. Resmi Lekshmi. Indian Institute of Space Science & Technology Trivandrum Gamma Ray Bursts Progress & Prospects Resmi Lekshmi Indian Institute of Space Science & Technology Trivandrum Why study GRBs? to study GRBs end stages of massive star evolution jet launching, collimation

More information

Formation and evolution of BH and accretion disk in Collapsar

Formation and evolution of BH and accretion disk in Collapsar Formation and evolution of BH and accretion disk in Collapsar Yuichiro Sekiguchi National Astronomical Observatory of Japan arxiv : 1009.5303 Motivation Collapsar model of GRB Central engine : Black hole

More information

Gamma-Ray Astronomy. Astro 129: Chapter 1a

Gamma-Ray Astronomy. Astro 129: Chapter 1a Gamma-Ray Bursts Gamma-Ray Astronomy Gamma rays are photons with energies > 100 kev and are produced by sub-atomic particle interactions. They are absorbed by our atmosphere making observations from satellites

More information

Black Hole Physics via Gravitational Waves

Black Hole Physics via Gravitational Waves Black Hole Physics via Gravitational Waves Image: Steve Drasco, California Polytechnic State University and MIT How to use gravitational wave observations to probe astrophysical black holes In my entire

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

From space-time to gravitation waves. Bubu 2008 Oct. 24

From space-time to gravitation waves. Bubu 2008 Oct. 24 From space-time to gravitation waves Bubu 008 Oct. 4 Do you know what the hardest thing in nature is? and that s not diamond. Space-time! Because it s almost impossible for you to change its structure.

More information

THIRD-YEAR ASTROPHYSICS

THIRD-YEAR ASTROPHYSICS THIRD-YEAR ASTROPHYSICS Problem Set: Stellar Structure and Evolution (Dr Ph Podsiadlowski, Michaelmas Term 2006) 1 Measuring Stellar Parameters Sirius is a visual binary with a period of 4994 yr Its measured

More information

A Relativistic Toy Model for Black Hole-Neutron Star Mergers

A Relativistic Toy Model for Black Hole-Neutron Star Mergers A Relativistic Toy Model for Francesco Pannarale A.Tonita, L.Rezzolla, F.Ohme, J.Read Max-Planck-Institute für Gravitationsphysik (Albert-Einstein-Institut) SFB Videoseminars, Golm - January 17, 2011 Introduction

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

Ref. PRL 107, (2011)

Ref. PRL 107, (2011) Kenta Kiuchi, Y. Sekiguchi, K. Kyutoku, M. Shibata Ref. PRL 107, 051102 (2011) Y TP YUKAWA INSTITUTE FOR THEORETICAL PHYSICS Introduction Coalescence of binary neutron stars Promising source of GWs Verification

More information

The Theory of Supernovae in Massive Binaries

The Theory of Supernovae in Massive Binaries The Theory of Supernovae in Massive Binaries Philipp Podsiadlowski (Oxford) the majority of massive stars are in interacting binaries the large diversity of observed supernova types and (sub-)types is

More information

Kozai-Lidov oscillations

Kozai-Lidov oscillations Kozai-Lidov oscillations Kozai (1962 - asteroids); Lidov (1962 - artificial satellites) arise most simply in restricted three-body problem (two massive bodies on a Kepler orbit + a test particle) e.g.,

More information

Massive star clusters

Massive star clusters Massive star clusters as a host of compact binaries Michiko Fujii ( 藤井通子 ) The University of Tokyo Outline Massive star clusters and compact binaries Dynamical evolution of star clusters Distribution of

More information

Gravitational Waves & Intermediate Mass Black Holes. Lee Samuel Finn Center for Gravitational Wave Physics

Gravitational Waves & Intermediate Mass Black Holes. Lee Samuel Finn Center for Gravitational Wave Physics Gravitational Waves & Intermediate Mass Black Holes Lee Samuel Finn Center for Gravitational Wave Physics Outline What are gravitational waves? How are they produced? How are they detected? Gravitational

More information

Fundamental Physics, Astrophysics and Cosmology with ET

Fundamental Physics, Astrophysics and Cosmology with ET Fundamental Physics, Astrophysics and Cosmology with ET B.S. Sathyaprakash (CU) and Bernard Schutz (CU, AEI) based on a Living Review article with a similar title (in preparation) ET Science Summary Fundamental

More information

Astrophysical Stochastic Gravitational Waves. Jonah Kanner PHYS 798G March 27, 2007

Astrophysical Stochastic Gravitational Waves. Jonah Kanner PHYS 798G March 27, 2007 Astrophysical Stochastic Gravitational Waves Jonah Kanner PHYS 798G March 27, 2007 Introduction Gravitational Waves come from space Require acceleration of dense mass (Think black holes and neutron stars!)

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

arxiv: v1 [astro-ph] 6 Aug 2007

arxiv: v1 [astro-ph] 6 Aug 2007 1 1. Introduction arxiv:0708.0696v1 [astro-ph] 6 Aug 2007 X-Ray binaries with neutron star accretors are traditionally divided in to two groups based on the massesofthe donorstars. One is low-massx-raybinaries(lmxbs)

More information

Unravelling the progenitors of merging black hole binaries

Unravelling the progenitors of merging black hole binaries Unravelling the progenitors of merging black hole binaries Dipartimento di Fisica e Astronomia G. Galilei, Università di Padova. INAF, Osservatorio Astronomico di Padova, Padova, Italy. INFN, Milano Bicocca,

More information

Gravitational Radiation from Coalescing SMBH Binaries in a Hierarchical Galaxy Formation Model

Gravitational Radiation from Coalescing SMBH Binaries in a Hierarchical Galaxy Formation Model Gravitational Radiation from Coalescing SMBH Binaries in a Hierarchical Galaxy Formation Model Motohiro ENOKI (National Astronomical Observatory of Japan) Kaiki Taro INOUE (Kinki University) Masahiro NAGASHIMA

More information

The Formation of the Most Relativistic Pulsar PSR J

The Formation of the Most Relativistic Pulsar PSR J Binary Radio Pulsars ASP Conference Series, Vol. 328, 2005 F. A. Rasio and I. H. Stairs The Formation of the Most Relativistic Pulsar PSR J0737 3039 B. Willems, V. Kalogera, and M. Henninger Northwestern

More information

Coalescing Binary Black Holes Originating from Globular Clusters

Coalescing Binary Black Holes Originating from Globular Clusters Coalescing Binary Black Holes Originating from Globular Clusters Abbas Askar (askar@camk.edu.pl) Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Warsaw, Poland Abbas Askar Globular

More information

Stellar Winds Jorick Vink (Keele University)

Stellar Winds Jorick Vink (Keele University) Stellar Winds Jorick Vink (Keele University) Outline Why predict Mass-loss rates? (as a function of Z) Monte Carlo Method Results O & B, LBV, B[e] & WR winds Cosmological implications? Why predict Mdot?

More information

Short gamma-ray bursts from binary neutron star mergers: the time-reversal scenario

Short gamma-ray bursts from binary neutron star mergers: the time-reversal scenario Short gamma-ray bursts from binary neutron star mergers: the time-reversal scenario Riccardo Ciolfi Physics Department, University of Trento INFN-TIFPA, Trento Institute for Fundamental Physics and Applications

More information

Synergy with Gravitational Waves

Synergy with Gravitational Waves Synergy with Gravitational Waves Alexandre Le Tiec and Jérôme Novak Laboratoire Univers et Théories Observatoire de Paris / CNRS LIGO, Virgo, ( elisa, ET,... ( What is a gravitational wave? A gravitational

More information

The Evolution of Close Binaries

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:

More information

Compact Binaries - 3 ASTR2110 Sarazin

Compact Binaries - 3 ASTR2110 Sarazin Compact Binaries - 3 ASTR2110 Sarazin Zoology of Binary Stars X-ray Binary Pulsar Spin-Up Accreted material has high angular momentum Spins up neutron star (true of ~all X-ray binary pulsars) Millisecond

More information

arxiv: v1 [astro-ph.sr] 4 Jul 2018

arxiv: v1 [astro-ph.sr] 4 Jul 2018 Astronomy & Astrophysics manuscript no. 33107corr c ESO 2018 July 5, 2018 Star-planet interactions V. Dynamical and equilibrium tides in convective zones Suvrat Rao 1, 2, Georges Meynet 1, Patrick Eggenberger

More information

Testing GR with Compact Object Binary Mergers

Testing GR with Compact Object Binary Mergers Testing GR with Compact Object Binary Mergers Frans Pretorius Princeton University The Seventh Harvard-Smithsonian Conference on Theoretical Astrophysics : Testing GR with Astrophysical Systems May 16,

More information

Gravity. Newtonian gravity: F = G M1 M2/r 2

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

More information

The Many Possible Histories of Globular Cluster Cores. John Fregeau (KITP), with Harvey Richer (UBC), Fred Rasio (NU), Jarrod Hurley (Swinburne)

The Many Possible Histories of Globular Cluster Cores. John Fregeau (KITP), with Harvey Richer (UBC), Fred Rasio (NU), Jarrod Hurley (Swinburne) The Many Possible Histories of Globular Cluster Cores John Fregeau (KITP), with Harvey Richer (UBC), Fred Rasio (NU), Jarrod Hurley (Swinburne) Two Parallel Threads The strong correlation between X-ray

More information

Jongsuk Hong (KIAA) MODEST /06/28. Collaborators: E. Vesperini, A. Askar, M. Giersz, M. Szkudlarek & T. Bulik

Jongsuk Hong (KIAA) MODEST /06/28. Collaborators: E. Vesperini, A. Askar, M. Giersz, M. Szkudlarek & T. Bulik Jongsuk Hong (KIAA) MODEST-18 2018/06/28 Collaborators: E. Vesperini, A. Askar, M. Giersz, M. Szkudlarek & T. Bulik Introduction Method & models BBH mergers & Host cluster properties Merger rate estimation

More information

The Stellar Graveyard

The Stellar Graveyard ASTR 1120 General Astronomy: Stars & Galaxies The Stellar Graveyard!EXT $ursday 10/15: #IDTERM #2!EXT Tuesday 10/20: "!earching for distant world"# GO DIRECTLY TO THE PLANETARIUM What s In The Stellar

More information

A synthetic model of the gravitational wave background from evolving binary compact objects

A synthetic model of the gravitational wave background from evolving binary compact objects A synthetic model of the gravitational wave background from evolving binary compact objects Irina Dvorkin, Jean-Philippe Uzan, Elisabeth Vangioni, Joe Silk (Institut d Astrophysique de Paris) [arxiv:1607.06818]

More information

arxiv: v2 [astro-ph.he] 4 Jan 2012

arxiv: v2 [astro-ph.he] 4 Jan 2012 DRAFT VERSION SEPTEMBER 27, 2018 Preprint typeset using LATEX style emulateapj v. 5/2/11 UNDERSTANDING COMPACT OBJECT FORMATION AND NATAL KICKS. III. THE CASE OF CYGNUS X-1 TSING-WAI WONG 1, FRANCESCA

More information

Mass Transfer in Binaries

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

More information

arxiv:astro-ph/ v1 17 Apr 1999

arxiv:astro-ph/ v1 17 Apr 1999 arxiv:astro-ph/9904224v1 17 Apr 1999 COALESCENCE RATES OF DOUBLE NEUTRON STARS V. KALOGERA Harvard-Smithsonian Center for Astrophysics, 60 Garden St., Cambridge, MA 02138, USA Merger events of close double

More information

The Stellar Graveyard

The Stellar Graveyard ASTR 101 General Astronomy: Stars & Galaxies The Stellar Graveyard NEXT Thursday 10/22: MIDTERM #2 What s In The Stellar Graveyard? Lower mass stars (M< 8Msun)! white dwarfs Gravity vs. electron degeneracy

More information

Confronting Theory with Gravitational Wave Observations

Confronting Theory with Gravitational Wave Observations Gravitation: A Decennial Perspective Confronting Theory with Gravitational Wave Observations B F Schutz Max Planck Institute for Gravitational Physics () Golm/Potsdam Germany The AEI congratulates The

More information

Dynamics of Stars and Black Holes in Dense Stellar Systems:

Dynamics of Stars and Black Holes in Dense Stellar Systems: Michela Mapelli INAF - Padova Dynamics of Stars and Black Holes in Dense Stellar Systems: Lecture V: STELLAR & INTERMEDIATE-MASS BLACK HOLES 0. stellar black holes (BHs) from star evolution 1. BHs as members

More information

Lobster X-ray Telescope Science. Julian Osborne

Lobster X-ray Telescope Science. Julian Osborne Lobster X-ray Telescope Science Julian Osborne What we want The whole high-energy sky right now 1.00E+13 1.00E+12 1 / f_lim (100 s) 1.00E+11 1.00E+10 1.00E+09 1.00E+08 0.0000001 0.000001 0.00001 0.0001

More information

Solar surface rotation

Solar surface rotation Stellar rotation Solar surface rotation Solar nearsurface rotation Surface Doppler Schou et al. (1998; ApJ 505, 390) Rotational splitting Inferred solar internal rotation Near solidbody rotation of interior

More information

Lecture 13: Binary evolution

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

More information

arxiv: v1 [astro-ph.sr] 14 Oct 2016

arxiv: v1 [astro-ph.sr] 14 Oct 2016 Nonconservative Mass Transfer in Massive Binaries and the Formation of Wolf-Rayet+O Binaries Yong Shao 1,2 and Xiang-Dong Li 1,2 arxiv:1610.04307v1 [astro-ph.sr] 14 Oct 2016 1 Department of Astronomy,

More information

Formation of low-mass X-ray Binaries with a BH accretor: challenging the paradigm

Formation of low-mass X-ray Binaries with a BH accretor: challenging the paradigm Formation of low-mass X-ray Binaries with a BH accretor: challenging the paradigm Semyon Chaichenets (UofA) Stephen Justham (KIAA, Beijing) John Fregeau (KITP, UCSB) Craig Heinke (UofA) Jamie Lombardi

More information

Superradiant sca.ering in astrophysical binary systems

Superradiant sca.ering in astrophysical binary systems Gr@v Superradiant sca.ering in astrophysical binary systems João G. Rosa University of Aveiro Phys. Le.. B749, 226 (2015) [arxiv:1501.07605 [gr- qc]] + work in progress VIII Black Holes Workshop, IST Lisbon,

More information

Averaging the average: Morphology transitions in spin precession of black-hole binaries

Averaging the average: Morphology transitions in spin precession of black-hole binaries Averaging the average: Morphology transitions in spin precession of black-hole binaries U. Sperhake DAMTP, University of Cambridge M. Kesden, D. Gerosa, R. O Shaughnessy, E. Berti VII Black Holes Workshop

More information

, G RAVITATIONAL-WAVE. Kent Yagi. with N. Yunes. Montana State University. YKIS2013, Kyoto

, G RAVITATIONAL-WAVE. Kent Yagi. with N. Yunes. Montana State University. YKIS2013, Kyoto UNIVERSAL I-LOVE OVE-Q Q RELATIONSR IN Q R NEUTRON STARS AND THEIR APPLICATIONS TO ASTROPHYSICS STROPHYSICS,, GRAVITATIONAL G RAVITATIONAL-WAVE AVE, G AND FUNDAMENTAL PHYSICS Kent Yagi with N. Yunes Montana

More information

The impact of reduced mass loss rates on

The impact of reduced mass loss rates on Clumping in Hot-Star Winds, Potsdam, June 2007 The impact of reduced mass loss rates on the evolution of massive stars Raphael HIRSCHI (KEELE University, UK) Plan 2 Introduction Impact of reduced mass

More information

Dr G. I. Ogilvie Lent Term 2005 INTRODUCTION

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

More information

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

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

More information

NS-NS and BH-NS Merger Simulations Lecture 3

NS-NS and BH-NS Merger Simulations Lecture 3 NS-NS and BH-NS Merger Simulations Lecture 3 Yuk Tung Liu ( 廖育棟 ) July 26-30, 2010 Asia Pacific Center for Theoretical Physics, Pohang (Korea) 2010 International School on Numerical Relativity and Gravitational

More information

Gravitational Waves & Related Studies (N6-WG3)

Gravitational Waves & Related Studies (N6-WG3) Gravitational Waves & Related Studies (N6-WG3) Kostas Kokkotas Department of Physics Aristotle University of Thessaloniki Greece Working Groups and financial Repartition: Overall annual budget ~100k Coordinator:

More information

How beaming of gravitational waves compares to the beaming of electromagnetic waves: impacts to gravitational wave detection

How beaming of gravitational waves compares to the beaming of electromagnetic waves: impacts to gravitational wave detection Journal of Physics: Conference Series PAPER OPEN ACCESS How beaming of gravitational waves compares to the beaming of electromagnetic waves: impacts to gravitational wave detection To cite this article:

More information

White Dwarf Binaries in Contact: Dynamical Stability at the Onset of Mass Transfer

White Dwarf Binaries in Contact: Dynamical Stability at the Onset of Mass Transfer White Dwarf Binaries in Contact: Dynamical Stability at the Onset of Mass Transfer Sterl Phinney* Caltech (*poor substitute for Danny Steeghs) KITP, Paths to Exploding Stars E.S. Phinney, 3/19/2007, 1

More information

General Relativistic MHD Simulations of Neutron Star Mergers

General Relativistic MHD Simulations of Neutron Star Mergers General Relativistic MHD Simulations of Neutron Star Mergers Luca Baiotti Osaka University with Luciano Rezzolla, Bruno Giacomazzo, Kentaro Takami Plan of the talk Brief overview of the status of BNS simulations

More information

Supernovae, Gamma-Ray Bursts, and Stellar Rotation

Supernovae, Gamma-Ray Bursts, and Stellar Rotation Supernovae, Gamma-Ray Bursts, and Stellar Rotation When Massive Stars Die, How Do They Explode? Neutron Star + Neutrinos Neutron Star + Rotation Black Hole + Rotation Colgate and White (1966) Arnett Wilson

More information

Formation and cosmic evolution of supermassive black holes. Debora Sijacki

Formation and cosmic evolution of supermassive black holes. Debora Sijacki Formation and cosmic evolution of supermassive black holes Debora Sijacki Summer school: Black Holes at all scales Ioannina, Greece, Sept 16-19, 2013 Lecture 1: - formation of black hole seeds - low mass

More information

Searching for Intermediate Mass Black Holes mergers

Searching for Intermediate Mass Black Holes mergers Searching for Intermediate Mass Black Holes mergers G. A. Prodi, Università di Trento and INFN for the LIGO Scientific collaboration and the Virgo collaboration special credits to Giulio Mazzolo and Chris

More information