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arXiv · 1302.5019

On the fate of the matter reinserted within young nuclear stellar clusters

Filiberto Hueyotl-Zahuantitla·Jan Palous·Richard Wunsch·Guillermo Tenorio-Tagle·Sergiy Silich
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Abstract

This paper presents a hydrodynamical model describing the evolution of the gas reinserted by stars within a rotating young nuclear star cluster (NSC). We explicitly consider the impact of the stellar component to the flow by means of a uniform insertion of mass and energy within the stellar cluster. The model includes the gravity force of the stellar component and a central supermassive black hole (SMBH), and accounts for the heating from the central source of radiation and the radiative cooling of the thermalized gas. By using a set of parameters typical for NSCs and SMBHs in Seyfert galaxies our simulations show that a filamentary/clumpy structure is formed in the inner part of the cluster. This "torus" is Compton thick and covers a large fraction of the sky (as seen from the SMBH). In the outer parts of the cluster a powerful wind is produced, that inhibits the infall of matter from larger scales and thus the NSC-SMBH interplay occurs in isolation.

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Filiberto Hueyotl-Zahuantitla, Jan Palous, Richard Wunsch, Guillermo Tenorio-Tagle, Sergiy Silich. 2013-02-20. On the fate of the matter reinserted within young nuclear stellar clusters. https://doi.org/10.1088/0004-637x/766/2/92

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