The physical origin of stellar envelopes around globular clusters
|
|
- Erick Perry
- 5 years ago
- Views:
Transcription
1 The physical origin of stellar envelopes around globular clusters Phil Breen University of Edinburgh in collaboration with A. L. Varri, J. Peñarrubia and D. C. Heggie
2 Current observational evidence Example: NGC 1851 Number density (Olszewski et al. 2009) Velocity dispersion (Marino et al. 2014)
3 Extra-tidal spherical envelopes Recent observations report the existence of diffuse spherical stellar envelopes extending few times r t. But what is r t? Name r t (pc) size (pc) mass % power law ref NGC ,3 NGC M Tuc ) Kuzma et al. 2016, 2) Kuzma et al. 2017, 3) Olszewski et al. 2009, 4) Piatti 2017 r t values from Harris 2010
4 King truncation radius? Some limitations of lowered isothermal models: Phase space truncation: different prescriptions provide different truncation radii. Independent of the Jacobi radius. (e.g., Mclaughlin & van der Marel 2005) Tidal filling: such models can often fit very underfilling (isolated) clusters, but resulting r t does not trace the real tidal limitation (e.g., Baumgardt et al.2010) Potential escapers: physical argument for an energy cut off doesn t account for spatially confined, unbound stars (e.g., Kuepper et al. 2010, Claydon et al. 2016) Kuepper et al 2010
5 Is there even an envelope? 10r t 5r t r t Jacobi radii based on apocentre and pericentre distances, from Balbinot & Gieles 2017 (calculated as in Ernst & Just 2002, assuming logarithmic Galactic potential)
6 More realistic tidal field The Jacobi surface is not spherical, and the flattening of equipotential surfaces is monotonically increasing with radius (e.g., Heggie & Ramamani1995)
7 Possible interpretations Classical interpretation: Tidal shocks/heating & potential escapers Alternative interpretation: Non-baryonic dark matter ( mini halos ) Modified gravity
8 Classical interpretation Stationary field (circular orbit): potentially large population of potential escapers filling the Jacobi surface (see Kuepper et al. 2010, Claydon et al. 2016) Time-variable field (elliptic, or more complex orbit): simple models indicate that disk shocks remove potential escapers, as they are more likely to be heated.
9 Alternative interpretation: external (or modified) potential Cosmological context and motivation: A possible cosmological formation scenario involves globular clusters forming in dark matter mini halos (e.g. Peebles 1984) These mini halos could have then been stripped by tidal forces in the inner regions of galaxies (Bromm & Clarke 2002, Mashchenko & Sills 2005 a,b) Another scenario is that (especially massive) globular clusters may be the remnants of tidally-stripped nucleated galaxies (e.g., Bekki & Yong 2012)
10 Populating stellar envelopes in an external potential Assuming the envelope is populated by ejection from the centre (i.e. radial orbits) (r) = f c 4 r 2 Z p 2(E N(E) )P (E) de Assuming smooth distribution of velocities Therefore we just need to know the potential (which constrains the period) to solve the integral above We can also reverse the problem, given a ρ we can solve for the envelope potential (within the assumptions) Big caveat: tidal effects currently not accounted for!
11 Dark matter - Keplerian potential Peñarrubia, Varri, Breen et al (arxiv: ) r -1 r -2 r -3 r -4 Theory predicts ~r -4 at large radii. Comparison with simple numerical experiments with tracer particles in cluster s + additional potential Equivalent argument in galactic context, linked to violent relaxation (see von Hoerner 1957, Bertin & Stiavelli 1983, Jaffe 1987, Makino 1990, Aguilar 2008)
12 Dark matter Uniform Density Background Theory predicts ~r -2 at large radii (flattening near edge of the sphere) Comparison with simple numerical experiments with tracer particles in cluster s + additional potential
13 MOND potential Models predicts ~r -2 at large radii for deep MOND regime In the Newtonian regime ~r -4 Comparison with simple numerical experiments with tracer particles in cluster s + additional potential
14 Self consistent N-body simulations Breen et al., in preparation (Too) simple theory confronted so far only with numerical experiments with tracer particles in static dark matter halo + cluster potential Next step : full collisional treatment of the cluster within a static dark matter potential. Crucial to explore evaporation vs. ejection behaviour. Modified Nbody6 (Aarseth 2003) to include a static dark matter potential (additional contribution to regular force). Experimented with several dark matter potentials.
15 Collisional dynamics within a dark matter potential Breen et al., in preparation Escapers Envelope stars Green bound to cluster, blue bound to cluster + DM (no tidal effects, for now)
16 Collisional dynamics within a dark matter potential Breen et al., in preparation Without DM Halo With DM Halo Many purely stellar dynamics questions, e.g. what happens to core collapse? It might not happen at all! And other surprises
17 Summary Growing interest for the structural and kinematic properties of the outskirts of globular clusters. High-quality kinematics is needed. Assessment of the tidal limitation should be done with care (a truncation radius is not the Jacobi radius!). Theoretical prediction that envelope stars are distributed with a slope that depends on the choice of the additional potential (dark matter/mond). Understanding of tidal effects in progress The presence of a dark matter potential can significantly change the dynamical evolution of collisional stellar systems (e.g. delayed core collapse). Much to explore and understand.
18 Additional Slides
19 Dark matter in globular clusters Baryonic component: 'dark remnants' White dwarfs, neutron stars, and stellar-mass black holes may make up a significant fraction of a cluster's mass (e.g., Heggie & Hut 1996) Sollima et al 2016
20 Internal kinematics - initial conditions Breen et al., in preparation Plummer model self-consistently embedded in a Hernquist DM halo The velocity dispersion increases as the dark matter halo mass increases, reducing the energy flux
21 Stellar envelopes in dark mini halos Peñarrubia, Varri, Breen et al. 2017, (arxiv: ) Red bound to cluster mass Blue bound to cluster plus dark matter halo Hernquist potential used for dark matter (i.e. -GM/(a+r))
Dynamical friction, galaxy merging, and radial-orbit instability in MOND
Dynamical friction, galaxy merging, and radial-orbit instability in MOND Carlo Nipoti Dipartimento di Astronomia Università di Bologna Strasbourg, 29 June 2010 Outline MOND and Equivalent Newtonian Systems
More informationStellar-mass black holes in a globular cluster. Douglas Heggie. University of Edinburgh, UK
Stellar-mass black holes in a globular cluster Douglas Heggie University of Edinburgh, UK d.c.heggie@ed.ac.uk How many stellar-mass black holes do you expect to find? Example: M4 Assume: initial conditions
More informationDirect N-body simulations of distant halo globular clusters
Direct N-body simulations of distant halo globular clusters Hosein Haghi Institute for Advanced Studies in Basic Sciences (IASBS) Zanjan, IRAN in collaboration with Akram Hasani Zonoozi (IASBS), Holger
More informationStellar 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 informationThe effect of primordial mass segregation on the size scale of the star clusters
The effect of primordial mass segregation on the size scale of the star clusters Hosein Haghi In collaboration with: HoseiniRad, Zonoozi, Kuepper Institute for Advanced Studies in Basic Sciences (IASBS),Zanjan
More informationKinetic 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 informationAS1001:Extra-Galactic Astronomy
AS1001:Extra-Galactic Astronomy Lecture 5: Dark Matter Simon Driver Theatre B spd3@st-andrews.ac.uk http://www-star.st-and.ac.uk/~spd3 Stars and Gas in Galaxies Stars form from gas in galaxy In the high-density
More informationarxiv: v2 [astro-ph.sr] 28 Apr 2017
Mon. Not. R. Astron. Soc. 000, 1 16 (2016) Printed 1 May 2017 (MN LATEX style file v2.2) arxiv:1612.02253v2 [astro-ph.sr] 28 Apr 2017 The properties of energetically unbound stars in stellar clusters Ian
More informationStellar-mass black holes in a globular cluster
Stellar-mass black holes in a globular cluster Douglas Heggie University of Edinburgh, UK d.c.heggie@ed.ac.uk Motivation Discovery of two stellar-mass BH in the Galactic globular cluster M22 (Strader+
More informationEvolution of Star Clusters on Eccentric Orbits
Evolution of Star Clusters on Eccentric Orbits Maxwell Xu CAI (NAOC/KIAA) Collaborators: Mark Gieles, Douglas Heggie, Anna Lisa Varri Cai et al. (2016), MNRAS, 455, 596 7th KCK meeting, NAOC, Dec 15, 2015
More informationarxiv:astro-ph/ v2 7 Oct 2004
Formation of ω Centauri by Tidal Stripping of a Dwarf Galaxy Makoto Ideta Astronomical Data Analysis Center, National Astronomical Observatory of Japan 2-21-1 Osawa, Mitaka, Tokyo 181-8588, Japan arxiv:astro-ph/0408431v2
More informationStellar Dynamics and Structure of Galaxies
Stellar Dynamics and Structure of Galaxies. Spherically symmetric objects Vasily Belokurov vasily@ast.cam.ac.uk Institute of Astronomy Lent Term 2016 1 / 21 Outline I 1 2 Globular of galaxies 2 / 21 Why
More informationVisible Matter. References: Ryden, Introduction to Cosmology - Par. 8.1 Liddle, Introduction to Modern Cosmology - Par. 9.1
COSMOLOGY PHYS 30392 DENSITY OF THE UNIVERSE Part I Giampaolo Pisano - Jodrell Bank Centre for Astrophysics The University of Manchester - March 2013 http://www.jb.man.ac.uk/~gp/ giampaolo.pisano@manchester.ac.uk
More informationInverting the dynamical evolution problem of globular clusters: clues to their origin
Inverting the dynamical evolution problem of globular clusters: clues to their origin Mark Gieles Poul Alexander (Cambridge), Douglas Heggie (Edinburgh) Alice Zocchi, Miklos Peuten, Vincent Hénault-Brunet
More informationEvolution of second generation stars in stellar disks of globular and nuclear clusters: ω Centauri as a test case
Evolution of second generation stars in stellar disks of globular and nuclear clusters: ω Centauri as a test case Alessandra Mastrobuono-Battisti & Hagai Perets Outline Dense stellar clusters: Nuclear
More informationEvolution of star clusters on eccentric orbits
doi:10.1093/mnras/stv2325 Evolution of star clusters on eccentric orbits Maxwell Xu Cai ( ), 1,2 Mark Gieles, 3 Douglas C. Heggie 4 and Anna Lisa Varri 4 1 National Astronomical Observatories of China,
More informationGaia 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 informationProbing Gravity in the Low Acceleration Regime with Globular Clusters
Probing Gravity in the Low Acceleration Regime with Globular Clusters By Riccardo Scarpa Instituto de astrofisica de Canarias Gran Telescopio Canarias The idea for this study sparked from the desire of
More informationDark matter and galaxy formation
Dark matter and galaxy formation Galaxy rotation The virial theorem Galaxy masses via K3 Mass-to-light ratios Rotation curves Milky Way Nearby galaxies Dark matter Baryonic or non-baryonic A problem with
More informationProbing Gravity in the Low Acceleration Regime with Globular Clusters
Probing Gravity in the Low Acceleration Regime with Globular Clusters By Riccardo Scarpa, Gianni Marconi & Roberto Gilmozzi European Southern Observatory The idea of this study sparked from the following
More informationarxiv: v1 [astro-ph.ga] 5 Oct 2015
Mon. Not. R. Astron. Soc. 000, 1?? (2015) Printed 4 September 2018 (MN LaT E X style file v2.2) arxiv:1510.01337v1 [astro-ph.ga] 5 Oct 2015 Evolution of star clusters on eccentric orbits Maxwell Xu Cai
More informationProbing Galaxy Halos with Tidal Interactions. Kyoto University Astronomy Department June 27, 2013
Probing Galaxy Halos with Tidal Interactions Kyoto University Astronomy Department June 27, 2013 Galaxy Formation Baryons cool & collapse in dark halo potentials. White & Rees 78 Galaxy Formation Baryons
More informationASTRON 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 informationDancing in the dark: spotting BHS & IMBH in GC
Dancing in the dark: spotting BHS & IMBH in GC ARI-ZAH, Heidelberg University Star Clusters around the Milky Way and in the Local Group Heidelberg August 15th-17th, 2018 Unravelling stellar black hole
More informationDwarf Galaxy Dispersion Profile Calculations Using a Simplified MOND External Field Effect
Dwarf Galaxy Dispersion Profile Calculations Using a Simplified MOND External Field Effect On the Shoulders of Giants Workshop Case Western Reserve University June 7, 2017 Stephen Alexander Physics Department
More informationGravitational Efects and the Motion of Stars
Gravitational Efects and the Motion of Stars On the largest scales (galaxy clusters and larger), strong evidence that the dark matter has to be non-baryonic: Abundances of light elements (hydrogen, helium
More informationThe structure and internal kinematics of globular clusters: tides and gravity
The structure and internal kinematics of globular clusters: tides and gravity Antonio Sollima Antonio.sollima@oapd.inaf.it Collaborators : C. Nipoti (Univ. Bo), D. Martinez-Delgado (MPIA), M. Bellazzini
More informationDynamical Models of the Globular Clusters M4 and NGC 6397
Dynamical Models of the Globular Clusters M4 and NGC 6397 Douglas Heggie University of Edinburgh d.c.heggie@ed.ac.uk in collaboration with Mirek Giersz CAMK, Warsaw, Poland Outline Introduction: M4 and
More informationarxiv: v1 [astro-ph.ga] 25 Oct 2009
**FULL TITLE** ASP Conference Series, Vol. **VOLUME**, c **YEAR OF PUBLICATION** **NAMES OF EDITORS** The Mass-to-Light Ratios of Galactic Globular Clusters arxiv:0910.4773v1 [astro-ph.ga] 25 Oct 2009
More informationStructure and substructure in dark matter halos
Satellites and Tidal Streams ING IAC joint Conference La Palma, May 2003 Structure and substructure in dark matter halos Simon D.M. White Max Planck Institute for Astrophysics 500 kpc A CDM Milky Way Does
More informationABSTRACT 1 INTRODUCTION
Mon. Not. R. Astron. Soc. 000, 1 11 (2015) Printed 24 September 2018 (MN LATEX style file v2.2) Back to the Future: Estimating Initial Globular Cluster Masses from their Present Day Stellar Mass Functions
More informationMassive 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 informationMichela Mapelli. LECTURES on COLLISIONAL DYNAMICS: 1. RELEVANT TIMESCALES, FORMATION OF STAR CLUSTERS, EQUILIBRIUM MODELS
Michela Mapelli LECTURES on COLLISIONAL DYNAMICS: 1. RELEVANT TIMESCALES, FORMATION OF STAR CLUSTERS, EQUILIBRIUM MODELS COLLISIONAL/COLLISIONLESS? Collisional systems are systems where interactions between
More informationBlack Hole Subsystems in Galactic Globular Clusters: Unravelling BH Populations in GCs using MOCCA Star Cluster Simulations
Black Hole Subsystems in Galactic Globular Clusters: Unravelling BH Populations in GCs using MOCCA Star Cluster Simulations Artist impression of a stellar mass BH detected in NGC 3201 (Giesers et al. 2018)
More informationPhys/Astro 689: Lecture 11. Tidal Debris
Phys/Astro 689: Lecture 11 Tidal Debris Goals (1) We ll explore whether we can trace the accretion events that should have formed the Milky Way. (2) We ll discuss the impact of tidal debris on direct detection
More informationComponents of Galaxies: Dark Matter
Components of Galaxies: Dark Matter Dark Matter: Any Form of matter whose existence is inferred solely through its gravitational effects. -B&T, pg 590 Nature of Major Component of Universe Galaxy Formation
More informationSurface Brightness of Spiral Galaxies
Surface Brightness of Spiral Galaxies M104: SA N4535: SAB LMC: dwarf irregular,barred Normal 1/4-law+exp fits An example of surface brightness profile. The top curve is the sum of exp disk+1/4-bulge. The
More informationDark Matter & Dark Energy. Astronomy 1101
Dark Matter & Dark Energy Astronomy 1101 Key Ideas: Dark Matter Matter we cannot see directly with light Detected only by its gravity (possible future direct detection in the lab) Most of the matter in
More informationMultiple populations in GCs: constraints on formation scenarios from kinematics & dynamics
Multiple populations in GCs: constraints on formation scenarios from kinematics & dynamics Vincent Hénault-Brunet Mark Gieles Oscar Agertz Justin Read Alice Zocchi IAU 316: Formation, evolution, and survival
More informationUsing globular clusters to test gravity in the weak acceleration regime
Using globular clusters to test gravity in the weak acceleration regime Riccardo Scarpa 1, Gianni Marconi 2, Roberto Gilmozzi 2, and Giovanni Carraro 3 1 Instituto de Astrofísica de Canarias, Spain 2 European
More informationarxiv: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 informationarxiv: v1 [astro-ph.ga] 21 Aug 2017
Draft version November 22, 2017 Typeset using LATEX twocolumn style in AASTeX61 DETECTION OF A DIFFUSE EXTENDED HALO-LIKE STRUCTURE AROUND 47 TUC Andrés E. Piatti 1, 2 arxiv:1708.06194v1 [astro-ph.ga]
More informationCo-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 informationThree Major Components
The Milky Way Three Major Components Bulge young and old stars Disk young stars located in spiral arms Halo oldest stars and globular clusters Components are chemically, kinematically, and spatially distinct
More informationGalaxies: Structure, Dynamics, and Evolution. Elliptical Galaxies (II)
Galaxies: Structure, Dynamics, and Evolution Elliptical Galaxies (II) Layout of the Course Feb 5: Review: Galaxies and Cosmology Feb 12: Review: Disk Galaxies and Galaxy Formation Basics Feb 19: Disk Galaxies
More informationThe Role of Dissipation in Spheroid Formation
The Role of Dissipation in Spheroid Formation Philip Hopkins 4/08/08 Lars Hernquist, TJ Cox, John Kormendy, Tod Lauer, Suvendra Dutta, Dusan Keres, Volker Springel Ellipticals & Bulges: Formation in Mergers?
More informationMOND and the Galaxies
MOND and the Galaxies Françoise Combes Observatoire de Paris With Olivier Tiret Angus, Famaey, Gentile, Wu, Zhao Wednesday 1st July 2009 MOND =MOdified Newtonian Dynamics Modification at weak acceleration
More informationASTR 200 : Lecture 22 Structure of our Galaxy
ASTR 200 : Lecture 22 Structure of our Galaxy 1 The 'Milky Way' is known to all cultures on Earth (perhaps, unfortunately, except for recent city-bound dwellers) 2 Fish Eye Lens of visible hemisphere (but
More informationMilky Way s Mass and Stellar Halo Velocity Dispersion Profiles
Milky Way s Mass and Stellar Halo Velocity Dispersion Profiles Shanghai Astronomical Observatory In collaboration with Juntai Shen, Xiang Xiang Xue, Chao Liu, Chris Flynn, Ling Zhu, Jie Wang Contents 1
More informationEnhancement of Antimatter Signals from Dark Matter Annihilation
Enhancement of Antimatter Signals from Dark Matter Annihilation around Intermediate Mass Black Holes Pierre Brun Laboratoire d Annecy-le-vieux de Physique des Particules CNRS/IN2P3/Université de Savoie
More informationSuperluminal neutrinos?
Superluminal neutrinos? Measurement of the neutrino velocity with the OPERA detector in the CNGS beam, T. Adam et al. 2011, arxiv:1109.4897v1: v > c by 2.48 x 10-5 Superluminal neutrinos? Neutrino velocity
More informationPhys/Astro 689: Lecture 8. Angular Momentum & the Cusp/Core Problem
Phys/Astro 689: Lecture 8 Angular Momentum & the Cusp/Core Problem Summary to Date We first learned how to construct the Power Spectrum with CDM+baryons. Found CDM agrees with the observed Power Spectrum
More informationGalaxy 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 informationCh. 25 In-Class Notes: Beyond Our Solar System
Ch. 25 In-Class Notes: Beyond Our Solar System ES2a. The solar system is located in an outer edge of the disc-shaped Milky Way galaxy, which spans 100,000 light years. ES2b. Galaxies are made of billions
More informationTHE MILKY WAY HALO. Wyn Evans Institute of Astronomy, Cambridge. Garching, 23 February 2015
THE MILKY WAY HALO Wyn Evans Institute of Astronomy, Cambridge Garching, 23 February 2015 THE STELLAR HALO The fundamental observation goes back half a century. Eggen, Lynden-Bell & Sandage (1962) noted
More information3 The lives of galaxies
Discovering Astronomy : Galaxies and Cosmology 24 3 The lives of galaxies In this section, we look at how galaxies formed and evolved, and likewise how the large scale pattern of galaxies formed. But before
More informationForming 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 informationView of the Galaxy from within. Lecture 12: Galaxies. Comparison to an external disk galaxy. Where do we lie in our Galaxy?
Lecture 12: Galaxies View of the Galaxy from within The Milky Way galaxy Rotation curves and dark matter External galaxies and the Hubble classification scheme Plotting the sky brightness in galactic coordinates,
More informationPoisson Equation. The potential-energy tensor. Potential energy: work done against gravitational forces to assemble a distribution of mass ρ(x)
Poisson Equation 1 2 Potential energy: work done against gravitational forces to assemble a distribution of mass ρ(x) The potential-energy tensor Assuming a distribution of mass is already in place, and
More informationKilling Dwarfs with Hot Pancakes. Frank C. van den Bosch (MPIA) with Houjun Mo, Xiaohu Yang & Neal Katz
Killing Dwarfs with Hot Pancakes Frank C. van den Bosch (MPIA) with Houjun Mo, Xiaohu Yang & Neal Katz The Paradigm... SN feedback AGN feedback The halo mass function is much steeper than luminosity function
More informationarxiv: v1 [astro-ph] 1 May 2008
Mon. Not. R. Astron. Soc. 000, 000 000 (0000) Printed 1 May 2008 (MN LATEX style file v2.2) Dynamical Evolution of the Mass Function and Radial Profile of the Galactic Globular Cluster System arxiv:0805.0058v1
More informationSummary So Far! M87van der Maerl! NGC4342! van den Bosch! rotation velocity!
Summary So Far Fundamental plane connects luminosity, scale length, surface brightness, stellar dynamics. age and chemical composition Elliptical galaxies are not randomly distributed within the 3D space
More informationAstrophysical observations preferring Modified Gravity
Astrophysical observations preferring Modified Gravity A natural approach to extended Newtonian gravity: tests and predictions across astrophysical scales. Mon.Not.Roy.Astron.Soc. 411 (2011) 226-234 Wide
More information2 Frederic A. Rasio. 2. Summary of Recent Results
2 Frederic A. Rasio dynamical evolution of a self-gravitating spherical cluster of N point masses whose orbits in the cluster are specified by an energy E and angular momentum J, with perturbations E and
More informationMOdelling DEnse STellar systems. A personal survey
MOdelling DEnse STellar systems A personal survey Douglas Heggie University of Edinburgh, UK d.c.heggie@ed.ac.uk Outline 0. Introduction 1. Tools of the trade 2. Tidal effects 3. Dynamics of binaries 0.
More informationChapter 15 The Milky Way Galaxy. The Milky Way
Chapter 15 The Milky Way Galaxy The Milky Way Almost everything we see in the night sky belongs to the Milky Way We see most of the Milky Way as a faint band of light across the sky From the outside, our
More informationMilky Way S&G Ch 2. Milky Way in near 1 IR H-W Rixhttp://online.kitp.ucsb.edu/online/galarcheo-c15/rix/
Why study the MW? its "easy" to study: big, bright, close Allows detailed studies of stellar kinematics, stellar evolution. star formation, direct detection of dark matter?? Milky Way S&G Ch 2 Problems
More informationNumerical 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 informationBlack Holes in Globular Clusters
Black Holes in Globular Clusters Douglas Heggie University of Edinburgh d.c.heggie@ed.ac.uk Papers on black holes and globular clusters Spot the odd man out Cen M15 www.jb.man.ac.uk The pioneer phase:
More informationActive 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 informationCosmologists dedicate a great deal of effort to determine the density of matter in the universe. Type Ia supernovae observations are consistent with
Notes for Cosmology course, fall 2005 Dark Matter Prelude Cosmologists dedicate a great deal of effort to determine the density of matter in the universe Type Ia supernovae observations are consistent
More informationClicker Question: Clicker Question: Clicker Question: Clicker Question: What is the remnant left over from a Type Ia (carbon detonation) supernova:
Test 3 results D C Grades posted in cabinet and Grades posted on-line B A F If you are not properly registered then come see me for your grade What is the ultimate origin of the elements heavier than helium
More informationThe formation and evolution of globular cluster systems. Joel Pfeffer, Nate Bastian (Liverpool, LJMU)
The formation and evolution of globular cluster systems Joel Pfeffer, Nate Bastian (Liverpool, LJMU) Introduction to stellar clusters Open clusters: few - 10 4 M few Myr - few Gyr solar metallicity disk
More informationDynamics of Stars and Black Holes in Dense Stellar Systems:
Michela Mapelli INAF - Padova Dynamics of Stars and Black Holes in Dense Stellar Systems: Lecture I: STAR CLUSTERS AS COLLISIONAL SYSTEMS 1. Relevant timescales of dense stellar systems 2. Early evolution
More informationDynamics of Stars and Black Holes in Dense Stellar Systems:
Michela Mapelli INAF - Padova Dynamics of Stars and Black Holes in Dense Stellar Systems: Lecture IV: Dynamical processes induced by mass spectrum 0. EFFECTS OF MASS SPECTRUM 1. MASS SEGREGATION 2. EQUIPARTITION
More informationModelling individual globular clusters An Update
Modelling individual globular clusters An Update Douglas Heggie University of Edinburgh d.c.heggie@ed.ac.uk Outline 1. Introduction: two kinds of model two kinds of star cluster 2. Monte Carlo models M4
More informationStellar Population Synthesis, a Discriminant Between Gravity Models
Stellar Population Synthesis, a Discriminant Between Gravity Models Akram Hasani Zonoozi Institute for Advanced Studies in Basic Sciences, IASBS Zanjan, Iran In collaboration with: H.Haghi & Y.Sobouti
More informationMonte Carlo Modelling of Globular Clusters
Monte Carlo Modelling of Globular Clusters Douglas Heggie University of Edinburgh d.c.heggie@ed.ac.uk Collaboration with Mirek Giersz (Warsaw) The globular cluster M4 Distance from sun Mass Core radius
More informationOutline. Walls, Filaments, Voids. Cosmic epochs. Jeans length I. Jeans length II. Cosmology AS7009, 2008 Lecture 10. λ =
Cosmology AS7009, 2008 Lecture 10 Outline Structure formation Jeans length, Jeans mass Structure formation with and without dark matter Cold versus hot dark matter Dissipation The matter power spectrum
More informationFeedback, 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 informationMasses of Dwarf Satellites of the Milky Way
Masses of Dwarf Satellites of the Milky Way Manoj Kaplinghat Center for Cosmology UC Irvine Collaborators: Greg Martinez Quinn Minor Joe Wolf James Bullock Evan Kirby Marla Geha Josh Simon Louie Strigari
More informationUCD forma*on in cosmological simula*ons
UCD forma*on in cosmological simula*ons Holger Baumgardt University of Queensland, Brisbane, Australia In collabora*on with Joel Pfeffer (UQ), Brendan Griffen (MIT), Michael Hilker (ESO) Ultra- compact
More informationarxiv:astro-ph/ v1 30 Nov 2004
Probing Halos with PNe: Mass and Angular Momentum in Early-Type Galaxies Aaron J. Romanowsky arxiv:astro-ph/0411797v1 30 Nov 2004 School of Physics and Astronomy, University of Nottingham, University Park,
More informationUMa II and the Orphan Stream
UMa II and the Orphan Stream M. Fellhauer The Cambridge Mafia Field of Streams Belokurov et al. 2006 A short The Bifurcation of the Sagittarius stream: (a typical Sagittarius like simulation) Fellhauer
More informationThe 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 informationDark Matter Density Function Depending on Gravitational Field as Universal Law - M. Abarca
DARK MATTER DENSITY FUNCTION DEPENDING ON INTENSITY OF GRAVITATIONAL FIELD AS UNIVERSAL LAW Author Manuel Abarca Hernández e-mail mabarcaher1@gmail.com INDEX 1. ABSTRAT.... INTRODUCTION... 4 3. GALACTIC
More informationOverview 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 informationThe Milky Way Galaxy
1/5/011 The Milky Way Galaxy Distribution of Globular Clusters around a Point in Sagittarius About 00 globular clusters are distributed in random directions around the center of our galaxy. 1 1/5/011 Structure
More informationdistribution of mass! The rotation curve of the Galaxy ! Stellar relaxation time! Virial theorem! Differential rotation of the stars in the disk
Today in Astronomy 142:! The local standard of rest the Milky Way, continued! Rotation curves and the! Stellar relaxation time! Virial theorem! Differential rotation of the stars in the disk distribution
More informationASTR 200 : Lecture 25. Galaxies: internal and cluster dynamics
ASTR 200 : Lecture 25 Galaxies: internal and cluster dynamics 1 Galaxy interactions Isolated galaxies are often spirals One can find small galaxy `groups' (like the Local group) with only a few large spiral
More informationDark Matter. 4/24: Homework 4 due 4/26: Exam ASTR 333/433. Today. Modified Gravity Theories MOND
Dark Matter ASTR 333/433 Today Modified Gravity Theories MOND 4/24: Homework 4 due 4/26: Exam Not any theory will do - length scale based modifications can be immediately excluded as the discrepancy does
More informationWhat can M2M do for Milky Way Models?
What can M2M do for Milky Way Models? Ortwin Gerhard Max-Planck-Institut für Extraterrestrische Physik, Garching gerhard@mpe.mpg.de Thanks to F. de Lorenzi, V. Debattista, P. Das, L. Morganti I. Made-to-Measure
More informationarxiv: v1 [astro-ph] 31 Jul 2007
Mon. Not. R. Astron. Soc. 000, 1?? (1994) Printed 1 February 8 (MN LATEX style file v1.4) Origin of lower velocity dispersions of ultra-compact dwarf galaxy populations in clusters of galaxies K. Bekki
More information1 [3 p.] First things first. 4 [2p.] Mass to light II. 5 [3p.] Merger remnants
Name and student number: [will be needed in the real exam] ASTC22 (GALACTIC AND EXTRAGALACTIC ASTROPHYSICS) PREPARATION SETFOR FINAL EXAM (#7) - PROBLEMS. SOLVED, SOME NOT. SOME FULLY Points in the square
More informationLecture 30. The Galactic Center
Lecture 30 History of the Galaxy Populations and Enrichment Galactic Evolution Spiral Arms Galactic Types Apr 5, 2006 Astro 100 Lecture 30 1 The Galactic Center The nature of the center of the Galaxy is
More informationDirect N-body simulations of globular clusters III. Palomar 4 on an eccentric orbit
Advance Access publication 2017 January 19 doi:10.1093/mnras/stx130 Direct N-body simulations of globular clusters III. Palomar 4 on an eccentric orbit Akram Hasani Zonoozi, 1 Hosein Haghi, 1 Pavel Kroupa,
More informationCoalescing 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 information25.2 Stellar Evolution. By studying stars of different ages, astronomers have been able to piece together the evolution of a star.
25.2 Stellar Evolution By studying stars of different ages, astronomers have been able to piece together the evolution of a star. Star Birth The birthplaces of stars are dark, cool interstellar clouds,
More informationCosmological Puzzles: Dwarf Galaxies and the Local Group
Cosmological Puzzles: Dwarf Galaxies and the Local Group Julio F. Navarro Dark-matter-only simulations have highlighted a number of cosmological puzzles Local Group puzzles Missing satellites problem Satellite
More informationSupermassive Black Holes
Supermassive Black Holes Leiden, Modern Research: Galaxy Formation and Evolution Tom van Leth & Maarten van Dijk November 25, 2005 1 Introduction Introduction Black hole theory Characteristics of SMBH
More information