Symmetries and Dynamics of Star Clusters

Result code in 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>
Result on the web
<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>

Result language
angličtina
Original language name
Symmetries and Dynamics of Star Clusters
Original language description
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
Czech name
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Czech description
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Project
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Continuities
I - Institucionalni podpora na dlouhodoby koncepcni rozvoj vyzkumne organizace

Publication year
2014
Confidentiality
S - Úplné a pravdivé údaje o projektu nepodléhají ochraně podle zvláštních právních předpisů

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