Symmetries and Dynamics of Star Clusters

Kód výsledku v IS VaVaI

<a href="https://www.isvavai.cz/riv?ss=detail&h=RIV%2F00216208%3A11320%2F14%3A10287240" target="_blank" >RIV/00216208:11320/14:10287240 - isvavai.cz</a>

Výsledek na webu

<a href="http://dx.doi.org/10.1007/978-3-319-03650-2" target="_blank" >http://dx.doi.org/10.1007/978-3-319-03650-2</a>

DOI - Digital Object Identifier

<a href="http://dx.doi.org/10.1007/978-3-319-03650-2" target="_blank" >10.1007/978-3-319-03650-2</a>

Jazyk výsledku

angličtina

Název v původním jazyce

Symmetries and Dynamics of Star Clusters

Popis výsledku v původním jazyce

We investigate the orbital evolution of an initially thin stellar disc around a supermassive black hole, considering various perturbative sources of gravity. By means of direct numerical N-body modelling, we first focus on the case when the disc is embedded in an extended spherically symmetric star cluster. We find that the gravitational influence of the disc triggers formation of macroscopic non-spherical substructure in the cluster which, subsequently, significantly affects the evolution of the disc itself. In another approximation, when the cluster is emulated by an analytic spherically symmetric potential, we further consider perturbative gravitational influence of a distant axisymmetric source. Using standard perturbation methods, we derive a simple semi-analytic model for such a configuration. It turns out that the additional axisymmetric potential leads to mutual gravitational coupling of the individual orbits from the disc. Consequently, the dense parts of the disc can, for som

Název v anglickém jazyce

Symmetries and Dynamics of Star Clusters

Popis výsledku anglicky

We investigate the orbital evolution of an initially thin stellar disc around a supermassive black hole, considering various perturbative sources of gravity. By means of direct numerical N-body modelling, we first focus on the case when the disc is embedded in an extended spherically symmetric star cluster. We find that the gravitational influence of the disc triggers formation of macroscopic non-spherical substructure in the cluster which, subsequently, significantly affects the evolution of the disc itself. In another approximation, when the cluster is emulated by an analytic spherically symmetric potential, we further consider perturbative gravitational influence of a distant axisymmetric source. Using standard perturbation methods, we derive a simple semi-analytic model for such a configuration. It turns out that the additional axisymmetric potential leads to mutual gravitational coupling of the individual orbits from the disc. Consequently, the dense parts of the disc can, for som

Druh

B - Odborná kniha

CEP obor

BN - Astronomie a nebeská mechanika, astrofyzika

OECD FORD obor

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Projekt

—

Návaznosti

I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Rok uplatnění

2014

Kód důvěrnosti údajů

S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

ISBN

978-3-319-03649-6

Počet stran knihy

79

Název nakladatele

Springer

Místo vydání

Cham

Kód UT WoS knihy

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