Dynamical evolution of rotating globular clusters with embedded black holes
In this dissertation evolution of self-gravitating dense stellar systems (e.g. globular clusters, galactic nuclei) with embedded black holes is investigated, motivated by observational evidences of the existence of central dark objects in these systems. The interaction between the stellar and black...
Gespeichert in:
| 1. Verfasser: | |
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| Dokumenttyp: | Book/Monograph Hochschulschrift |
| Sprache: | Deutsch Englisch |
| Veröffentlicht: |
2006
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| Schlagworte: | |
| Online-Zugang: | Verlag, Volltext: http://nbn-resolving.de/urn:nbn:de:bsz:16-opus-61459 Verlag, Volltext: http://d-nb.info/978929497/34 Verlag, Volltext: http://archiv.ub.uni-heidelberg.de/volltextserver/volltexte/2006/6145/index.html 
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| Verfasserangaben: | José Fiestas |
MARC
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| 245 | 1 | 0 | |a Dynamical evolution of rotating globular clusters with embedded black holes |c José Fiestas |
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| 520 | |a In this dissertation evolution of self-gravitating dense stellar systems (e.g. globular clusters, galactic nuclei) with embedded black holes is investigated, motivated by observational evidences of the existence of central dark objects in these systems. The interaction between the stellar and black hole component is followed in a way, different from most other investigations in this field, as flattening of the system due to differential rotation is allowed. The axisymmetric system is modelled using 2-dimensional, in energy and z-component of angular momentum, Fokker Planck numerical methods. The interplay between velocity diffusion due to relaxation and black hole star accretion is followed together with cluster rotation. The results show how angular momentum transport andstar accretion support the development of central rotation in relaxation time scales. Gravogyro and gravothermal instabilities conduce the system to a faster evolution leading to shorter collapsetimes with respect to models without black hole, and a faster cluster dissolution in the galactic tidal field of a parent galaxy. As a further application, two-dimensional distribution (in the meridional plane) of kinematical and structural parameters (density, dispersions, rotation) are reproduced, covering a wide range of ages, rotation, concentrations and ellipticities, with the aim toenable the use of set of models for comparison with observational data. | ||
| 520 | |a Diese Dissertation befasst sich mit der Untersuchung der Entwicklung selbstgravitierender dichter Sternsystemen (Kugelsternhaufen, aktive Galaxienkerne) mit einem zentralen Schwarzes-Loch, motiviert durch Beochachtungshinweise \"{u}ber die Existenz Schwarze L\"{o}cher in diesen Sternsysteme. Die Wechselwirkung zwischen Stern- und\\ Schwarzes-Loch-Komponente is verfolgt von einem Standpunkt, der sich von den meisten Untersuchungen in diesem Gebiet unterscheidet, da eine Abflachung des Systems is durch differentielle Rotationerm\"{o}glicht. Das axysimmetrische System is simuliert unter Verwendung zwei-dimensionaler, in Energie und Drehimpuls in z-Richtung, Fokker-Planck numerische Methoden. Die Wechselwirkung zwischen Diffusionprozesse und Sternenakkretion durch das Schwarze Loch ist verfolgt, unter dem Einfluss von Rotation. Die Ergebnisse zeigen wie Drehimpulstransport und Sternenakkretion unterst\"{u}tzen die Entstehung zentraler Rotation in Zeitskalen der Relaxation. Gravogyro und gravothermische Instabilit\"{a}ten f\"{u}hren zu einer schnelleren Entwicklung in kurzen Kollapszeiten in Bezug auf Modelle ohne Schwarzes-Loch, und schliesslich zu einer schnelleren Aufl\"{o}sung des Sternhaufens im Tidenfeld der Muttergalaxie. Eine weitere Anwendung ist die Erstellung zwei-Dimensionale Verteilungen (in der meridionalen Ebene) kinematischer und Strukturparametern (Dichte, Dispersion, Rotation) in einen breiten Alter-, Rotation-, Konzentration- und Elliptizit\"{a}ts-Wertebereich, mit dem Ziel der Verwendung theoretischer Modelle zum Vergleich mit Beobachtungsdata. | ||
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