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Massive Black Holes in Galaxies

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Massive Black Holes in Galaxies Michael Brockamp Massive Black Holes in Galaxies Massive Black Holes in Galaxies Dissertation zur Erlangung des Doktorgrades (Dr. rer. nat.) der Mathematisch-Naturwissenschaftlichen Fakult¨at der Rheinischen Friedrich-Wilhelms-Universit¨at Bonn vorgelegt von Michael Brockamp aus G¨utersloh Bonn, Juli 2014 Angefertigt mit Genehmigung der Mathematisch-Naturwissenschaftlichen Fakult¨at der Rheinischen Friedrich-Wilhelms-Universit¨at Bonn 1. Gutachter: Prof. Dr. Pavel Kroupa 2. Gutachter: Prof. Dr. Holger Baumgardt Tag der Promotion: 29.9.2014 Erscheinungsjahr: 2014 Erkl¨arung Ich versichere, daß ich die von mir vorgelegte Dissertation selbstst¨andig angefertigt, die benutzten Quellen und Hilfsmittel vollst¨andig angegeben und die Stellen der Arbeit - einschließlich Tabellen, Karten und Abbildungen -, die anderen Werken im Wortlaut oder dem Sinn nach entnommen sind, in jedem Einzelfall als Entlehnung kenntlich gemacht habe; daß diese Dissertation noch keiner anderen Fakult¨at oder Universit¨at zur Pr¨ufung vorgelegen hat; daß sie - abgesehen von unten angegeben Erstautor-Publikationen - noch nicht ver¨offentlicht worden ist sowie, daß ich eine solche Ver¨offentlichung vor Abschluß des Promotionsverfahrens nicht vornehmen werde. Die Bestimmungen dieser Promotionsordnung sind mir bekannt. Die von mir vorgelegte Dissertation ist von Prof. Dr. Pavel Kroupa betreut worden. Bonn, Datum , (Michael Brockamp) Erstautor-Publikationen Brockamp, M., Baumgardt, H., & Kroupa, P. 2011, MNRAS, 418, 1308 (Kapitel 3 in dieser Dissertation) Brockamp, M., K¨upper, A. H. W., Thies, I., Baumgardt, H., & Kroupa, P. 2014, MNRAS, 441, 150 (Kapitel 4 in dieser Dissertation) Weitere Publikationen Mieske, S., K¨upper, A. H. W., & Brockamp, M. 2014, A&A, 565, L6 Peuten, M., Brockamp, M., K¨upper, A. H. W., & Kroupa, P. 2014, ApJ, in press Zusammenfassung Die vorliegende Doktorarbeit handelt von supermassereichen schwarzen L¨ochern (SMSL), ihrem Wachstum und dem Einfluss, den sie auf ihre Wirtsgalaxien und deren Kugelsternhaufensysteme aus¨uben. Um die geleistete Arbeit in einen umfassenden wissenschaftlichen Kontext einordnen zu k¨onnen, werden im ersten Teil dieser Dok- torarbeit die relevanten wissenschaftlichen Grundlagen dargelegt. Gleichzeitig wird ein umfangreicher Uberblick¨ ¨uber den gegenw¨artigen Stand der Forschung schwarzer L¨ocher vermittelt. Zun¨achst wird im Rahmen der allgemeinen Relativit¨atstheorie die Physik dieser Objekte betrachtet (Kapitel 1). Dabei wird auf eine aktuelle Arbeit von Andrew Hamilton Bezug genommen. Diese gestattet es, Eigenschaften schwarzer L¨ocher anschaulich und zugleich mathematisch korrekt zu erl¨autern. Im Anschluss werden alle m¨oglichen Bahnen in einer Schwarzschild Metrik diskutiert auf denen sich Objekte bewegen k¨onnen. So wird eine Verbindung zwischen der Physik schwarzer L¨ocher und den Prozessen, die zu ihrem Wachstum f¨uhren, hergestellt. Diverse SMSL Wachstumsprozesse werden erl¨autert (Kapitel 2), nachdem auf beobachtbare Skalierungsrelationen eingegangen wurde. So enth¨alt die Steigung, aber auch die statistische Streuung dieser empirischen SMSL Skalierungsrelationen, wertvolle Infor- mationen ¨uber den Ursprung und das Wachstum schwarzer L¨ocher. Im zweiten Teil dieser Doktorarbeit (Kapitel 3) stehen die Ergebnisse der eigenen Forschung im Vordergrund. Zun¨achst wird ein Wachstumsprozess betrachtet, bei dem Sterne durch Relaxation im Drehimpulsraum zu Trajektorien hin diffundieren, welche letztendlich im unmittelbaren Einflussbereich des SMSL m¨unden. Die Sterne werden dabei von Gezeitenkr¨aften zerrissen und ein Teil der stellaren Materie wird akkretiert. Bei der verwendeten Methode handelt es sich um direkte N-K¨orperrechnungen. Es wird gezeigt, dass die Einfallrate von Sternen nicht hoch genug ist, um das Wachstum sehr massereicher schwarzer L¨ocher signifikant zu beeinflussen. Dennoch k¨onnen von SMSL zerrupfte Sterne einen erheblichen Anteil am Wachstum schwarzer L¨ocher im unteren Massenbereich von 104-105M beigetragen haben. Interessanterweise scheint ⊙ die Masse des SMSL keinen großen Einfluss auf die Einfallrate von Sternen zu haben. Die Ergebnisse wurden im MNRAS Journal publiziert. Im darauf folgenden Kapitel 4 wird eine selbstentwickelte Software vorgestellt, welche den Einfluss von Galaxien, zentralen schwarzen L¨ochern und weiteren Ef- fekten auf die Erosionsrate von Kugelsternhaufensystemen untersucht. Zum ersten Mal konnte eine weitreichende Verallgemeinerung der dynamischen Reibungsformel von Chandrasekhar eingebaut werden. Diese basiert nicht mehr auf der Annahme einer Maxwellschen Geschwindigkeitsverteilung. Des Weiteren ber ¨ucksichtigt sie, dass der Beschleunigungsvektor der dynamischen Reibung nicht anti-parallel zum v Geschwindigkeitsvektor stehen muss. Bereits in den ersten Rechnungen mit dieser Software haben sich Hinweise auf eine neue Phase in der Entwicklung von Kugel- sternhaufensystemen finden lassen. So wird anf¨anglich eine große Anzahl von Kugelsternhaufen durch starke Gezeitenschocks innerhalb der Galaxie zerst¨ort. Der Einfluss massereicher schwarzer L¨ocher auf die zeitliche Erosionsrate und Gesam- tanzahl zerst¨orter Kugelsternhaufen wird diskutiert. Dar ¨uberhinaus lassen sich die flachen Anzahldichteprofile von Kugelsternhaufensystemen in elliptischen Galaxien, sowie das Nichtvorhandensein von Kugelsternhaufen in der kompakten Zwerggalaxie M 32, einer Satellitengalaxie der Andromedagalaxie, erkl¨aren. Die Ergebnisse wurden in einem zweiten Artikel im MNRAS Journal ver¨offentlicht. Im dritten und letzten Teil dieser Doktorarbeit wird zun¨achst die numerische Im- plementierung eines schwarzen Loches inklusive voll relativistischer Einfangbedin- gungen erl¨autert. Anhand der relativistischen Perihel-Pr¨azession des Merkurs und dem Verschmelzungsprozess zweier schwarzer L¨ocher getestet, wird die Strategie zur Durchf¨uhrung eines weiteren, zuk¨unftigen Projektes mit dieser Software vorgestellt. Dabei geht es um das Wachstum massereicher schwarzer L¨ocher durch stellare Tr¨ummerteile von erodierten Sternhaufen. Schlussendlich wird auch noch die Bedeu- tung bereits gewonnener Erkenntnisse f¨ur die sogenannte spezifische Frequenz von Kugelsternhaufen in elliptischen Galaxien diskutiert. vi Summary The main subjects of the underlying PhD study are supermassive black holes (SMBHs), their growth and the influence they exert on vast globular cluster systems. In the first part of this work I provide a comprehensive overview of black hole related research. In this way the own findings can be connected to a broader scientific background. Simultaneously, the current state of SMBH research is summarized. The physics behind black holes will be presented first (Chapter 1). This is done by introduc- ing a fully general relativistic concept for visualizing black holes. It was developed by Andrew Hamilton. Afterwards, I will discuss all possible trajectories in a non-rotating Schwarzschild metric. In this way the link between the physics of black holes and various SMBH growth processes, which belong to the domain of astrophysics, can be established. However, before summarizing different growth scenarios, the most important scaling relations are described (Chapter 2). The slope and intrinsic scatter of these empirical correlations contain information about the SMBH growth history. In the second part of this PhD study I focus on my own results. In Chapter 3, I will investigate the flux of stars which enter loss cone trajectories through angular momen- tum diffusion. The inferred results are based on direct N-body computations which are presented in Brockamp et al. (2011). Depending on the mass of the central SMBH, stars on loss cone orbits can either be swallowed as a whole, or tidally disrupted. In the latter case some fraction of the unbounded star becomes accreted. It is found that the tidal disruption rate of stars is nearly independent of the SMBH mass. Angular momentum diffusion is not sufficient to fuel the growth of the most massive black holes. However, it can influence the growth history of SMBHs in the lowest mass range spanning 104-105M . ⊙ In the following Chapter 4 I present a newly developed computer code, which is called MUESLI. It numerically integrates the equation of motion of individual globular clusters (GCs) in elliptical galaxies by taking GC disruption processes into account. MUESLI thus evaluates the erosion rate of whole globular cluster systems. Several aspects which influence the GC erosion rate like the tidal field of the host galaxy, SMBHs and dynamical friction (DF) are considered. For the first time an extensive generalization of Chandrasekhar‘s dynamical friction formula is implemented into N-body software. It does not only handle non-Maxwellian velocity distributions, but can also treat dynamical friction forces which are not anti-parallel to the velocity vector. Already the first computations indicated a new phase in the evolution of whole globular cluster systems. Depending on the strength of the tidal field of the host galaxy, a huge fraction of GCs is destroyed rapidly through tidal shocking. The influence of the central SMBH on the fraction of destroyed GCs is discussed. Additionally, the vii performed computations naturally explain the central shallow number density profiles of GCs systems as well as the non existence of GCs around the compact dwarf galaxy M 32, which is a satellite of the Andromeda galaxy. The presented results are based on Brockamp et al. (2014). The implementation of a relativistic SMBH with fully general relativistic capture con- ditions into
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