Black Hole Mergers at Galactic. The Final Parsec: Supermassive. Centers. Milos Milosavljevic. California Institute of Technology

Size: px
Start display at page:

Download "Black Hole Mergers at Galactic. The Final Parsec: Supermassive. Centers. Milos Milosavljevic. California Institute of Technology"

Transcription

1 The Final Parsec: Supermassive Black Hole Mergers at Galactic Centers Milos Milosavljevic California Institute of Technology

2 MBH Binaries Form in Galaxy Mergers Borne et al 2000 by transferring binding energy and angular momentum to the ambient medium

3 GALAXY MERGER hard binary a hard G ( M = 8 + σ 1 2 M 2 ) black hole mass (solar mass) binary s semi-major axis (parsec)

4 ) 10 G Gyr ( M 1 + a hard = 8 σ 2 M c a t gr ~ 3 64 G M M ( M M ) 1 2 F ( e ) COALESCENCE black hole mass (solar mass) binary s semi-major axis (parsec)

5 The Final Parsec Problem GALAXY MERGER Can the binaries cover this? binary s semi-major axis (parsec) COALESCENCE black hole mass (solar mass)

6 Interaction of MBHB with Environment Stellar dynamics Dynamical friction Gravitational slingshot interaction Response of the stellar system Gas dynamics Economy of a QSO / AGN / star forming nucleus Accretion disks Multiple MBH / IMBH Gravitational slingshot interaction Resonances (Kozai, etc.)

7 Stellar Dynamics Initial Conditions: Phase Space Structure ρ ~ r 2 power-law core Gebhardt et al 1996 luminosity density luminosity density radius radius and Merger Dynamics Wechsler et al 2002

8 Major Mergers Proceed on a Dynamical Time Scale σ 1 σ 2 The merger time scale at a given separation depends on the stellar mass bound to the black holes >> M bh

9 The Minor Mergers are a Bottleneck t DF ~ (σ 1 /σ 2 ) 3 t dyn In shallow cusps, the smaller MBH is stripped bare of its stars

10 Gravitational Slingshot Mechanism The velocity of ejection scales as, but need not equal, the binary s orbital velocity v eject ~ v bin ~ (GM bin /a) 1/2 The velocity can increase or decrease, but preferentially increases Re-ejection and the potential well depth

11 Merger Finish Marks Start of Long Term Evolution orbital mass ~ 10 binary masses Simulations show that the binary rapidly shrinks by the factor of x10 from after v bin exceeds σ

12 The Loss Cone circular orbit Definition: Domain in phase space consisting of orbits strongly perturbed by individual components of a MBH binary Analogy with the loss cone for the tidal disruption of stars & the capture of compact objects energy However: The binary loss cone is much more extensive and does not destroy stars angular momentum

13 Diffusion into The Loss Cone E = const energy Equilibrium diffusion: Lightman & Shapiro 1977 Cohn & Kulsrud 1978, etc. Magorrian & Tremaine 1999 Yu 2002 GC Galaxies It can take more than a Hubble time to reach the state of equilibrium, particularly in intermediate and massive galaxies angular momentum

14 The Loss Cone: An Initial Value Problem Energy R L / L c ( E N t = µ 2 R ) N Heat equation in cylindrical coordinates The loss cone boundary Angular Momentum

15 Loss Cone Out of Equilibrium 1 Myr 10 Myr 100 Myr 1 Gyr 10 Gyr number of stars angular momentum actual loss cone profile profile in collisional equilibrium

16 Episodic Refilling? E.g. Zhao, Haehnelt, & Rees 2002 log(l) loss cone refilled loss cone refilled N(L) separation Satellite/star cluster infall Star formation episode log(l) time N(L)

17 Spherical Galaxy: Evolution of the Semi-Major Axis Loss cone always full 1 a t Loss cone partially full a 1 N α t α, 1 3 (Makino 1997) Loss cone almost empty a 1 1 N t Large-N limit Re-ejection only a 1 constant 1 a ln ( 1 + β t ) + γ Stalling? (MM & Merritt 2002)

18 Details The binary formation must be simulated. N-body simulations provide: Orbital parameters of the binary (a, e) Initial damage to the stellar cusp Geometry & kinematics of the new cusp Convergence is difficult With N<10 7-8, the simulations lack sufficient resolution due to the spurious relaxation and the spurious Brownian motion (to date, N<10 6 ) Latest, successful effort: Makino & Funato 2003 w/grape

19 Details (Cont d) Non-spherical loss cones add complexity, enhance the flux of stars entering Axisymmetry (e.g., Magorrian & Tremaine 1999, Yu 2002) Triaxiality (Merritt & Poon 2003 Time-dependent potentials (real galaxies!) (fig. J. Barnes)

20 Details (Cont d) Semi-analytic modeling of the binary decay requires detailed scattering data Basic elements studied via 3-body scattering (Hills 1980s, Quinlan 1996, etc.) The special case with equal black holes and a spherical loss cone is fairly well understood Eccentricity remains small Ejected mass ~ few times M bin Dynamics of unequal mass binaries & their effect on the galaxy structure have not been adequately studied

21 Observed Galaxies When photometric data are available, the distribution of stars near the loss cone cannot be determined without knowing the binary s age & the history of the stellar environment. Inferences about the binary separation based on the present-day luminosity profiles potentially underestimate the past decay rate, when the stellar cusp could have been denser.

22 The Mass Deficit γ min = 2.0 γ min =1.75 Definition: Mass that had to be removed to produce the observed profile from the fiducial pure power-law. γ min =1.5 MM, Merritt, Rest & van den Bosch 2001

23 Gas Dynamics Additional physics: dissipation, magnetic fields and star formation γ

24 The First Simulation! Escala, Larson, Coppi & Mardones 2003

25

26 Migration (A protoplanetary disk!) Ivanov, Papaloizou & Polnarev 1999 Armitage & Natarajan 2002 Goodman & Tan 2003 Levin 2003 Armitage & Natarajan 2002

27 Conclusions Idealized stellar dynamical models suggest that long-lived massive black hole binaries are generically produced in the mergers of intermediate and massive galaxies. Massive black hole binaries that form in mergers of low-mass galaxies coalesce in a Hubble time due to stellar dynamical processes. All established physical mechanisms aid an efficient coalescence of the black holes. Physical conditions in the nuclei of perturbed (merging, gas rich) galaxies are not well known, but progress is expected soon!

The Worst-Case Scenario. The Final Parsec Problem. and. Milos Milosavljevic. California Institute of Technology. Collaborator: David Merritt

The Worst-Case Scenario. The Final Parsec Problem. and. Milos Milosavljevic. California Institute of Technology. Collaborator: David Merritt The Final Parsec Problem and The Worst-Case Scenario Milos Milosavljevic California Institute of Technology Collaborator: David Merritt NSF AST 00-71099 NASA NAG5-6037, NAG5-9046 Sherman Fairchild Foundation

More information

The so-called final parsec problem

The so-called final parsec problem The so-called final parsec problem most galaxies contain black holes at their centers black-hole mass is 10 6-10 10 solar masses or roughly 0.2-0.5% of the stellar mass of the host galaxy galaxies form

More information

Evolution of SMBH-SMBH and SMBH-IMBH Binaries: Effect of Large Mass Ratio

Evolution of SMBH-SMBH and SMBH-IMBH Binaries: Effect of Large Mass Ratio Evolution of SMBH-SMBH and SMBH-IMBH Binaries: Effect of Large Mass Ratio Jun Makino Center for Computational Astrophysics and Division Theoretical Astronomy National Astronomical Observatory of Japan

More information

Astrophysics with LISA

Astrophysics with LISA Astrophysics with LISA Alberto Vecchio University of Birmingham UK 5 th LISA Symposium ESTEC, 12 th 15 th July 2004 LISA: GW telescope LISA is an all-sky monitor: All sky surveys are for free Pointing

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 VI: DYNAMICS AROUND SUPER-MASSIVE BHs 0. nuclear star clusters (NSCs) 1. dynamics around super-massive

More information

Forming Intermediate-Mass Black Holes in Dense Clusters Through Collisional Run-away

Forming Intermediate-Mass Black Holes in Dense Clusters Through Collisional Run-away Forming Intermediate-Mass Black Holes in Dense Clusters Through Collisional Run-away Marc Freitag ARI, Heidelberg freitag@ari.uni-heidelberg.de http://obswww.unige.ch/~freitag Collaboration with Atakan

More information

arxiv:astro-ph/ v1 30 Aug 2000

arxiv:astro-ph/ v1 30 Aug 2000 Dynamics of Star Clusters and the Milky Way ASP Conference Series, Vol. 000, 2000 S. Deiters, B. Fuchs, A. Just, R. Spurzem, and R. Wielen, eds. Dynamics of Black-Hole Nuclei arxiv:astro-ph/0008497v1 30

More information

Evolution of binary supermassive black holes via chain regularization

Evolution of binary supermassive black holes via chain regularization Rochester Institute of Technology RIT Scholar Works Presentations and other scholarship 2005 Evolution of binary supermassive black holes via chain regularization Andras Szell David Merritt Seppo Mikkola

More information

Major questions in postgalaxy merger evolution

Major questions in postgalaxy merger evolution Major questions in postgalaxy merger evolution Marta Volonteri Institut d Astrophysique de Paris Thanks to: Tamara Bogdanovic Monica Colpi Massimo Dotti Massive Black Holes and galaxies Massive Black Holes

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

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

arxiv:astro-ph/ v2 4 Oct 2004

arxiv:astro-ph/ v2 4 Oct 2004 Interaction of Supermassive Black Holes with their Stellar and Dark Matter Environments David Merritt Rochester Institute of Technology, Rochester, NY, USA arxiv:astro-ph/0409290v2 4 Oct 2004 1 Introduction

More information

Relativistic loss-cone dynamics: Implications for the Galactic Center

Relativistic loss-cone dynamics: Implications for the Galactic Center Relativistic loss-cone dynamics: Implications for the Galactic Center Relativistic loss-cone dynamics: Implications for the Galactic Center Tal Alexander Weizmann Institute of cience 3 RR < NR Plunge log

More information

Observational Signatures of Merging Black Holes (in galactic nuclei)

Observational Signatures of Merging Black Holes (in galactic nuclei) Observational Signatures of Merging Black Holes (in galactic nuclei) E. Sterl Phinney Caltech Dynamical masses of nuclear BH van den Bosch+ 2012 Entire galaxy! Phases of Black Hole merger Log(Time to Merger)

More information

Co-Evolution of Central Black Holes and Nuclear Star Clusters

Co-Evolution of Central Black Holes and Nuclear Star Clusters Co-Evolution of Central Black Holes and Nuclear Star Clusters Oleg Gnedin (University of Michigan) Globular clusters in the Galaxy median distance from the center is 5 kpc Resolved star cluster highest

More information

Feedback, AGN and galaxy formation. Debora Sijacki

Feedback, AGN and galaxy formation. Debora Sijacki Feedback, AGN and galaxy formation Debora Sijacki Formation of black hole seeds: the big picture Planck data, 2013 (new results 2015) Formation of black hole seeds: the big picture CMB black body spectrum

More information

Dual and Binary MBHs and AGN: Connecting Dynamics and Accretion

Dual and Binary MBHs and AGN: Connecting Dynamics and Accretion Dual and Binary MBHs and AGN: Connecting Dynamics and Accretion Sandor Van Wassenhove Marta Volonteri Lucio Mayer Jillian Bellovary Massimo Dotti Simone Callegari BH-Galaxy Coevolution Black holes found

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

Overview spherical accretion

Overview spherical accretion Spherical accretion - AGN generates energy by accretion, i.e., capture of ambient matter in gravitational potential of black hole -Potential energy can be released as radiation, and (some of) this can

More information

The Lagrange Points in a Binary BH System: Applications to Electromagnetic Signatures Jeremy Schnittman

The Lagrange Points in a Binary BH System: Applications to Electromagnetic Signatures Jeremy Schnittman The Lagrange Points in a Binary BH System: Applications to Electromagnetic Signatures Jeremy Schnittman NASA Goddard Space Flight Center RIT CCRG Seminar November 22, 2010 Motivation Observing supermassive

More information

AST Cosmology and extragalactic astronomy. Lecture 20. Black Holes Part II

AST Cosmology and extragalactic astronomy. Lecture 20. Black Holes Part II AST4320 - Cosmology and extragalactic astronomy Lecture 20 Black Holes Part II 1 AST4320 - Cosmology and extragalactic astronomy Outline: Black Holes Part II Gas accretion disks around black holes, and

More information

ASTRON 449: Stellar (Galactic) Dynamics. Fall 2014

ASTRON 449: Stellar (Galactic) Dynamics. Fall 2014 ASTRON 449: Stellar (Galactic) Dynamics Fall 2014 In this course, we will cover the basic phenomenology of galaxies (including dark matter halos, stars clusters, nuclear black holes) theoretical tools

More information

Numerical Investigations of a New N-Body Simulation Method

Numerical Investigations of a New N-Body Simulation Method International Journal of Astronomy and Astrophysics, 2012, 2, 119-124 http://dx.doi.org/10.4236/ijaa.2012.23016 Published Online September 2012 (http://www.scirp.org/journal/ijaa) Numerical Investigations

More information

Gaia Revue des Exigences préliminaires 1

Gaia Revue des Exigences préliminaires 1 Gaia Revue des Exigences préliminaires 1 Global top questions 1. Which stars form and have been formed where? - Star formation history of the inner disk - Location and number of spiral arms - Extent of

More information

Probing Massive Black Hole Binaries with the SKA. Alberto Sesana Albert Einstein Institute, Golm

Probing Massive Black Hole Binaries with the SKA. Alberto Sesana Albert Einstein Institute, Golm Probing Massive Black Hole Binaries with the SKA Alberto Sesana Albert Einstein Institute, Golm Alberto Vecchio University of Birmingham OUTLINE > MBH assembly > GW detection with PTAs > Signal characterization:

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

arxiv:astro-ph/ v2 12 Sep 2005

arxiv:astro-ph/ v2 12 Sep 2005 Massive Black Hole Binary Evolution arxiv:astro-ph/0410364v2 12 Sep 2005 David Merritt Rochester Institute of Technology Rochester, NY USA e-mail:david.merritt@rit.edu http://www.rit.edu/ drmsps/ Miloš

More information

Supermassive black hole hierarchical evolution. NASA/CXC animation

Supermassive black hole hierarchical evolution. NASA/CXC animation Supermassive black hole hierarchical evolution NASA/CXC animation Outline 1. SMBHs in the local universe: where from? 2. SMBHs Mass Growth: Accretion vs Merging AGN at low redshift 3. Dynamical Evolution

More information

Gravitational Wave Background Radiation from Supermassive Black Hole Binaries on Eccentric Orbits

Gravitational Wave Background Radiation from Supermassive Black Hole Binaries on Eccentric Orbits Gravitational Wave Background Radiation from Supermassive Black Hole Binaries on Eccentric Orbits Motohiro ENOKI (National Astronomical Observatory of Japan) & Masahiro NAGASHIMA (Nagasaki University)

More information

The Origin of Supermassive Black Holes. Daniel Whalen. McWilliams Fellow Carnegie Mellon

The Origin of Supermassive Black Holes. Daniel Whalen. McWilliams Fellow Carnegie Mellon The Origin of Supermassive Black Holes Daniel Whalen McWilliams Fellow Carnegie Mellon Mergers Accretion The SMBH Conundrum SDSS quasars of ~ 10 9 Msun have been found at z ~ 6, a Gyr after the Big Bang

More information

Simulating the mass assembly history of Nuclear Star Clusters

Simulating the mass assembly history of Nuclear Star Clusters Simulating the mass assembly history of Nuclear Star Clusters The imprints of cluster inspirals Alessandra Mastrobuono-Battisti Sassa Tsatsi Hagai Perets Nadine Neumayer Glenn vad de Ven Ryan Leyman David

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

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

The dynamical evolution of massive black hole binaries - II. Self-consistent N-body integrations.

The dynamical evolution of massive black hole binaries - II. Self-consistent N-body integrations. The dynamical evolution of massive black hole binaries - II. Self-consistent N-body integrations. Gerald D. Quinlan 1 and Lars Hernquist 2 1 Dept. of Physics and Astronomy, Rutgers University, PO Box 849,

More information

Upcoming class schedule

Upcoming class schedule Upcoming class schedule Thursday March 15 2pm AGN evolution (Amy Barger) th Monday March 19 Project Presentation (Brad) nd Thursday March 22 postponed to make up after spring break.. Spring break March

More information

Peculiar (Interacting) Galaxies

Peculiar (Interacting) Galaxies Peculiar (Interacting) Galaxies Not all galaxies fall on the Hubble sequence: many are peculiar! In 1966, Arp created an Atlas of Peculiar Galaxies based on pictures from the Palomar Sky Survey. In 1982,

More information

The Interplay Between Galaxies and Black Holes A Theoretical Overview. Massimo Ricotti (U of Maryland)

The Interplay Between Galaxies and Black Holes A Theoretical Overview. Massimo Ricotti (U of Maryland) The Interplay Between Galaxies and Black Holes A Theoretical Overview Massimo Ricotti (U of Maryland) ..a tale of many sleepless nights Maya and Noemi Ricotti Cosmological Context Outline Formation of

More information

I. Basic Goals. Most galaxies are in approx. equilibrium in the present-day universe.

I. Basic Goals. Most galaxies are in approx. equilibrium in the present-day universe. Elements of Galaxy Dynamics I. Basic Goals Most galaxies are in approx. equilibrium in the present-day universe. What equilibrium i solutions exist and which h are stable? A solution entails: in which

More information

arxiv: v1 [astro-ph.ga] 14 Jan 2019

arxiv: v1 [astro-ph.ga] 14 Jan 2019 Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 16 January 2019 (MN LATEX style file v2.2) Evolution of supermassive black hole binaries and tidal disruption rates in nonspherical galactic nuclei

More information

Laser Interferometer Space Antenna double black holes: dynamics in gaseous nuclear discs

Laser Interferometer Space Antenna double black holes: dynamics in gaseous nuclear discs Mon. Not. R. Astron. Soc. 367, 103 112 (2006) doi:10.1111/j.1365-2966.2005.09956.x Laser Interferometer Space Antenna double black holes: dynamics in gaseous nuclear discs Massimo Dotti, 1 Monica Colpi

More information

Fundamental Planes and Galaxy Formation

Fundamental Planes and Galaxy Formation Fundamental Planes and Galaxy Formation Philip Hopkins, NoviCosmo 2007 Fundamental Planes = Scaling Laws Obeyed by Galaxies vs Origin of scaling laws: Ideally, we d understand every galaxy as an individual:

More information

Thus Far. Intro / Some Definitions Hubble Classification Components of Galaxies. Specific Galaxy Types Star Formation Clusters of Galaxies

Thus Far. Intro / Some Definitions Hubble Classification Components of Galaxies. Specific Galaxy Types Star Formation Clusters of Galaxies Thus Far Intro / Some Definitions Hubble Classification Components of Galaxies Stars Gas Dust Black Holes Dark Matter Specific Galaxy Types Star Formation Clusters of Galaxies Components of Galaxies:

More information

Black Holes and Active Galactic Nuclei

Black Holes and Active Galactic Nuclei Black Holes and Active Galactic Nuclei A black hole is a region of spacetime from which gravity prevents anything, including light, from escaping. The theory of general relativity predicts that a sufficiently

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

Gravitational Potential Energy. The Gravitational Field. Grav. Potential Energy Work. Grav. Potential Energy Work

Gravitational Potential Energy. The Gravitational Field. Grav. Potential Energy Work. Grav. Potential Energy Work The Gravitational Field Exists at every point in space The gravitational force experienced by a test particle placed at that point divided by the mass of the test particle magnitude of the freefall acceleration

More information

Black Hole Coalescence: The Gravitational Wave Driven Phase

Black Hole Coalescence: The Gravitational Wave Driven Phase Black Hole Coalescence: The Gravitational Wave Driven Phase NASA Goddard UM Black Holes Augest 24, 2011 Motivation Observing supermassive black hole mergers will teach us about Relativity High-energy Astrophysics

More information

The Effects of Stellar Collisions in Dense Environments

The Effects of Stellar Collisions in Dense Environments The Effects of Stellar Collisions in Dense Environments Kevin France Department of Physics and Astronomy, Johns Hopkins University, Baltimore, MD 21218 france@pha.jhu.edu ABSTRACT Direct stellar collisions

More information

Sources of Gravitational Waves

Sources of Gravitational Waves 1 Sources of Gravitational Waves Joan Centrella Laboratory for High Energy Astrophysics NASA/GSFC Gravitational Interaction of Compact Objects KITP May 12-14, 2003 A Different Type of Astronomical Messenger

More information

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

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

More information

X-shaped radio galaxies as observational evidence for the interaction of supermassive binary black holes and accretion disc at parsec scale

X-shaped radio galaxies as observational evidence for the interaction of supermassive binary black holes and accretion disc at parsec scale Mon. Not. R. Astron. Soc. 347, 1357 1369 (2004) X-shaped radio galaxies as observational evidence for the interaction of supermassive binary black holes and accretion disc at parsec scale F. K. Liu Astronomy

More information

arxiv:astro-ph/ v1 7 Aug 2006

arxiv:astro-ph/ v1 7 Aug 2006 Draft version May 17, 2008 Preprint typeset using L A TEX style emulateapj v. 6/22/04 SATELLITE ACCRETION ONTO MASSIVE GALAXIES WITH CENTRAL BLACK HOLES Michael Boylan-Kolchin 1 and Chung-Pei Ma 2 Draft

More information

Active Galactic Nuclei-I. The paradigm

Active Galactic Nuclei-I. The paradigm Active Galactic Nuclei-I The paradigm An accretion disk around a supermassive black hole M. Almudena Prieto, July 2007, Unv. Nacional de Bogota Centers of galaxies Centers of galaxies are the most powerful

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

Overview of Dynamical Modeling. Glenn van de Ven

Overview of Dynamical Modeling. Glenn van de Ven Overview of Dynamical Modeling Glenn van de Ven glenn@mpia.de 1 Why dynamical modeling? -- mass total mass stellar systems key is to their evolution compare luminous mass: constrain DM and/or IMF DM radial

More information

Galaxy interaction and transformation

Galaxy interaction and transformation Galaxy interaction and transformation Houjun Mo April 13, 2004 A lot of mergers expected in hierarchical models. The main issues: The phenomena of galaxy interaction: tidal tails, mergers, starbursts When

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

Two Phase Formation of Massive Galaxies

Two Phase Formation of Massive Galaxies Two Phase Formation of Massive Galaxies Focus: High Resolution Cosmological Zoom Simulation of Massive Galaxies ApJ.L.,658,710 (2007) ApJ.,697, 38 (2009) ApJ.L.,699,L178 (2009) ApJ.,725,2312 (2010) ApJ.,744,63(2012)

More information

Inconvenient Tales of Dinosaurs

Inconvenient Tales of Dinosaurs Inconvenient Tales of Dinosaurs D. Richstone Univ of Michigan Thanks to key collaborators: Tod Lauer, Sandy Faber, Karl Gebhardt, Kayhan Gultekin, John Kormendy, Scott Tremaine And thanks to NASA Black

More information

Galaxy Dynamics Galaxies Block Course 2008 Hans-Walter Rix - MPIA

Galaxy Dynamics Galaxies Block Course 2008 Hans-Walter Rix - MPIA Galaxy Dynamics Galaxies Block Course 2008 Hans-Walter Rix - MPIA For more detail on any of this Binney and Tremaine, 1996 Binney and Merrifield, 2002 1 Basic Goals of Stellar Dynamics Most Empirical:

More information

Collisionless loss-cone refilling: there is no final parsec problem

Collisionless loss-cone refilling: there is no final parsec problem Advance Access publication 2016 October 4 doi:10.1093/mnras/stw2528 Collisionless loss-cone refilling: there is no final parsec problem Alessia Gualandris, 1 Justin I. Read, 1 Walter Dehnen 2 and Elisa

More information

Stellar Dynamics of Massive Blackhole Binaries

Stellar Dynamics of Massive Blackhole Binaries Stellar Dynamics of Massive Blackhole Binaries Jun Makino Center for Computational Astrophysics and Division Theoretical Astronomy National Astronomical Observatory of Japan Talk structure Brief overview

More information

Formation Processes of IMBHs

Formation Processes of IMBHs Formation Processes of IMBHs Melvyn B. Davies Department of Astronomy and Theoretical Physics Lund University www.astro.lu.se Stellar mass Intermediate mass SMBH (A) (B) Runaway collisions... Runaway mergers

More information

Kinematical evidence for an intermediate-mass black hole in M54

Kinematical evidence for an intermediate-mass black hole in M54 Kinematical evidence for an intermediate-mass black hole in M54 Eva Noyola Max-Planck Institute for Extraterrestrial Physics Collaborators: Karl Gebhardt & Marcel Bergmann History and motivation for finding

More information

The Star Clusters of the Magellanic Clouds

The Star Clusters of the Magellanic Clouds The Dance of Stars MODEST-14 The Star Clusters of the Magellanic Clouds Eva K. Grebel Astronomisches Rechen-Institut Zentrum für Astronomie der Universität Heidelberg Star Clusters in the Magellanic Clouds!

More information

FORMATION OF SUPERMASSIVE BLACK HOLES Nestor M. Lasso Cabrera

FORMATION OF SUPERMASSIVE BLACK HOLES Nestor M. Lasso Cabrera FORMATION OF SUPERMASSIVE BLACK HOLES Nestor M. Lasso Cabrera In this presentation the different theories that can explain the formation of Supermassive Black Holes (SMBH) are presented. Before focus on

More information

The Black Hole in the Galactic Center. Eliot Quataert (UC Berkeley)

The Black Hole in the Galactic Center. Eliot Quataert (UC Berkeley) The Black Hole in the Galactic Center Eliot Quataert (UC Berkeley) Why focus on the Galactic Center? The Best Evidence for a BH: M 3.6 10 6 M (M = mass of sun) It s s close! only ~ 10 55 Planck Lengths

More information

Star systems like our Milky Way. Galaxies

Star systems like our Milky Way. Galaxies Galaxies Star systems like our Milky Way Galaxies Contain a few thousand to tens of billions of stars,as well as varying amounts of gas and dust Large variety of shapes and sizes Gas and Dust in

More information

Chapter 21 Galaxy Evolution. How do we observe the life histories of galaxies?

Chapter 21 Galaxy Evolution. How do we observe the life histories of galaxies? Chapter 21 Galaxy Evolution How do we observe the life histories of galaxies? Deep observations show us very distant galaxies as they were much earlier in time (old light from young galaxies). 1 Observing

More information

arxiv:astro-ph/ v1 14 Oct 2003

arxiv:astro-ph/ v1 14 Oct 2003 **TITLE** ASP Conference Series, Vol. **VOLUME***, **YEAR OF PUBLICATION** **NAMES OF EDITORS** Galaxy threshing and the origin of intracluster stellar objects arxiv:astro-ph/0310350v1 14 Oct 2003 Kenji

More information

arxiv:astro-ph/ v2 15 Jan 2007

arxiv:astro-ph/ v2 15 Jan 2007 Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 16 January 2007 (MN LATEX style file v2.2) A hypervelocity star from the Large Magellanic Cloud Alessia Gualandris 1 and Simon Portegies Zwart 1 1

More information

Can black holes be formed in dynamic interactions in star clusters?

Can black holes be formed in dynamic interactions in star clusters? Can black holes be formed in dynamic interactions in star clusters? Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences Warsaw, Poland mig@camk.edu.pl MODEST 14 Workshop Bad Honnef, Germany

More information

How do Black Holes Get Their Gas?

How do Black Holes Get Their Gas? How do Black Holes Get Their Gas? Philip Hopkins Eliot Quataert, Lars Hernquist, T. J. Cox, Kevin Bundy, Jackson DeBuhr, Volker Springel, Dusan Keres, Gordon Richards, Josh Younger, Desika Narayanan, Paul

More information

The Milky Way nuclear star cluster: theoretical perspective. Structure Formation Evolution. Eugene Vasiliev

The Milky Way nuclear star cluster: theoretical perspective. Structure Formation Evolution. Eugene Vasiliev The Milky Way nuclear star cluster: theoretical perspective Structure Formation Evolution Eugene Vasiliev Institute of Astronomy, Cambridge Survival of dense star clusters in the Milky Way system Heidelberg,

More information

Pulsars as probes for the existence of IMBHs

Pulsars as probes for the existence of IMBHs Universidad de Valencia 15 November 2010 Pulsars as probes for the existence of IMBHs ANDREA POSSENTI Layout Known Black Hole classes Formation scenarios for the IMBHs IMBH candidates IMBH candidates (?)

More information

arxiv:astro-ph/ v2 14 Jul 2007

arxiv:astro-ph/ v2 14 Jul 2007 Intermediate and Extreme Mass-Ratio Inspirals Astrophysics, Science Applications and Detection using LISA arxiv:astro-ph/0703495v2 14 Jul 2007 Pau Amaro-Seoane 1, Jonathan R. Gair 2, Marc Freitag 2, M.

More information

Set 3: Galaxy Evolution

Set 3: Galaxy Evolution Set 3: Galaxy Evolution Environment. Galaxies are clustered, found in groups like the local group up to large clusters of galaxies like the Coma cluster Small satellite galaxies like the LMC and SMC are

More information

Stellar Dynamics and Structure of Galaxies

Stellar Dynamics and Structure of Galaxies Stellar Dynamics and Structure of Galaxies Gerry Gilmore H47 email: gil@ast.cam.ac.uk Lectures: Monday 12:10-13:00 Wednesday 11:15-12:05 Friday 12:10-13:00 Books: Binney & Tremaine Galactic Dynamics Princeton

More information

Measuring Black Hole Masses in Nearby Galaxies with Laser Guide Star Adaptive Optics

Measuring Black Hole Masses in Nearby Galaxies with Laser Guide Star Adaptive Optics Measuring Black Hole Masses in Nearby Galaxies with Laser Guide Star Adaptive Optics Claire Max Anne Medling Mark Ammons UC Santa Cruz Ric Davies Hauke Engel MPE-Garching Image of NGC 6240: Bush et al.

More information

Comparison of Simulated and Observational Catalogs of Hypervelocity Stars in Various Milky Way Potentials

Comparison of Simulated and Observational Catalogs of Hypervelocity Stars in Various Milky Way Potentials Comparison of Simulated and Observational Catalogs of Hypervelocity Stars in Various Milky Way Potentials Shannon Grammel under the direction of Dr. Paola Rebusco Massachusetts Institute of Technology

More information

The dynamics of neutron star and black hole binaries in young star clusters

The dynamics of neutron star and black hole binaries in young star clusters Michela Mapelli INAF-Osservatorio Astronomico di Padova The dynamics of neutron star and black hole binaries in young star clusters Collaborators: Mario Spera, Brunetto, Marica Branchesi, Alessandro Trani,

More information

arxiv: v1 [astro-ph.ga] 4 Jun 2015

arxiv: v1 [astro-ph.ga] 4 Jun 2015 DRAFT VERSION NOVEMBER 13, 2018 Preprint typeset using L A TEX style emulateapj v. 5/2/11 SUPPRESSION OF STELLAR TIDAL DISRUPTION RATES BY ANISOTROPIC INITIAL CONDITIONS KIRILL LEZHNIN 1 AND EUGENE VASILIEV

More information

Growing and merging massive black holes

Growing and merging massive black holes Growing and merging massive black holes Marta Volonteri Institut d Astrophysique de Paris S. Cielo (IAP) R. Bieri (MPA) Y. Dubois (IAP) M. Habouzit (Flatiron Institute) T. Hartwig (IAP) H. Pfister (IAP)

More information

Announcement: Quiz Friday, Oct 31

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

More information

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

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

More information

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

Kinetic Theory. Motivation - Relaxation Processes Violent Relaxation Thermodynamics of self-gravitating system

Kinetic Theory. Motivation - Relaxation Processes Violent Relaxation Thermodynamics of self-gravitating system Kinetic Theory Motivation - Relaxation Processes Violent Relaxation Thermodynamics of self-gravitating system negative heat capacity the gravothermal catastrophe The Fokker-Planck approximation Master

More information

In a dense region all roads lead to a black Hole (Rees 1984 ARAA) Deriving the Mass of SuperMassive Black Holes

In a dense region all roads lead to a black Hole (Rees 1984 ARAA) Deriving the Mass of SuperMassive Black Holes In a dense region all roads lead to a black Hole (Rees 1984 ARAA) Deriving the Mass of SuperMassive Black Holes Stellar velocity fields MW Distant galaxies Gas motions gas disks around nearby black holes

More information

SUPPLEMENTARY INFORMATION for Disruption of a Proto-Planetary Disk by the Black Hole at the Milky Way Centre. Ruth A. Murray-Clay & Abraham Loeb

SUPPLEMENTARY INFORMATION for Disruption of a Proto-Planetary Disk by the Black Hole at the Milky Way Centre. Ruth A. Murray-Clay & Abraham Loeb SUPPLEMENTARY INFORMATION for Disruption of a Proto-Planetary Disk by the Black Hole at the Milky Way Centre Ruth A. Murray-Clay & Abraham Loeb 1 Supplementary Figures Supplementary Figure S1: Dynamical

More information

Constraints on alternatives to supermassive black holes

Constraints on alternatives to supermassive black holes Mon. Not. R. Astron. Soc. 367, L32 L36 (2006) doi:10.1111/j.1745-3933.2006.00135.x Constraints on alternatives to supermassive black holes M. Coleman Miller 1,2 1 University of Maryland, Department of

More information

Active Galactic Nuclei

Active Galactic Nuclei Active Galactic Nuclei Optical spectra, distance, line width Varieties of AGN and unified scheme Variability and lifetime Black hole mass and growth Geometry: disk, BLR, NLR Reverberation mapping Jets

More information

Demographics of radio galaxies nearby and at z~0.55. Are radio galaxies signposts to black-hole mergers?

Demographics of radio galaxies nearby and at z~0.55. Are radio galaxies signposts to black-hole mergers? Elaine M. Sadler Black holes in massive galaxies Demographics of radio galaxies nearby and at z~0.55 Are radio galaxies signposts to black-hole mergers? Work done with Russell Cannon, Scott Croom, Helen

More information

Starbursts, AGN, and Interacting Galaxies 1 ST READER: ROBERT GLEISINGER 2 ND READER: WOLFGANG KLASSEN

Starbursts, AGN, and Interacting Galaxies 1 ST READER: ROBERT GLEISINGER 2 ND READER: WOLFGANG KLASSEN Starbursts, AGN, and Interacting Galaxies 1 ST READER: ROBERT GLEISINGER 2 ND READER: WOLFGANG KLASSEN Galaxy Interactions Galaxy Interactions Major and Minor Major interactions are interactions in which

More information

Evolution of Massive Black Hole Binaries in Rotating Stellar Nuclei and its Implications for Gravitational Wave Detection

Evolution of Massive Black Hole Binaries in Rotating Stellar Nuclei and its Implications for Gravitational Wave Detection Rochester Institute of Technology RIT Scholar Works Theses Thesis/Dissertation Collections 8-7-2017 Evolution of Massive Black Hole Binaries in Rotating Stellar Nuclei and its Implications for Gravitational

More information

arxiv: v1 [astro-ph.ga] 29 Sep 2016

arxiv: v1 [astro-ph.ga] 29 Sep 2016 Preprint 27 July 2018 Compiled using MNRAS LATEX style file v3.0 Collisionless loss-cone refilling: there is no final parsec problem arxiv:1609.09383v1 [astro-ph.ga] 29 Sep 2016 Alessia Gualandris 1, Justin

More information

Dark Matter Substructure and their associated Galaxies. Frank C. van den Bosch (MPIA)

Dark Matter Substructure and their associated Galaxies. Frank C. van den Bosch (MPIA) Dark Matter Substructure and their associated Galaxies Frank C. van den Bosch (MPIA) Outline PART I: The Subhalo Mass Function (van den Bosch, Tormen & Giocoli, 2005) PART II: Statistical Properties of

More information

Binary star formation

Binary star formation Binary star formation So far we have ignored binary stars. But, most stars are part of binary systems: Solar mass stars: about 2 / 3 are part of binaries Separations from: < 0.1 au > 10 3 au Wide range

More information

Binary Black Holes: An Introduction

Binary Black Holes: An Introduction Binary Black Holes: An Introduction Roger Blandford KIPAC Stanford 29 xi 2012 Tucson 1 Inertial Confinement of Extended Radio Sources Three Dimensional Magnetohydrodynamic Simulations of Buoyant Bubbles

More information

Stellar Black Hole Binary Mergers in Open ClusterS

Stellar Black Hole Binary Mergers in Open ClusterS Stellar Black Hole Binary Mergers in Open ClusterS SARA RASTELLO Collaborators: P. Amaro-Seoane, M. Arca-Sedda, R. Capuzzo Dolcetta, G. Fragione, I.Tosta e Melo Modest 18, Santorini, greece 27/06/2018

More information

Supermassive Black Hole Formation in Galactic Nuclei

Supermassive Black Hole Formation in Galactic Nuclei Supermassive Black Hole Formation in Galactic Nuclei Melvyn B. Davies Department of Astronomy and Theoretical Physics Lund University Ross Church (Lund), Cole Miller (Maryland), Serge Nzoke (Lund), Jillian

More information

More on Galaxy Classifcation

More on Galaxy Classifcation More on Galaxy Classifcation Trends within the Hubble Sequence E0 --> S0 --> Sb Decreasing bulge to disk ratio Decreasing stellar age Increasing gas content Increasing star formation rate Problems Constructed

More information