Hostname: page-component-586b7cd67f-dlnhk Total loading time: 0 Render date: 2024-11-26T22:24:04.410Z Has data issue: false hasContentIssue false

m=1 mode instabilities in nuclear stellar disks around black holes

Published online by Cambridge University Press:  01 December 2004

M. R. de Oliveira
Affiliation:
Instituto de Informática – UFRGS, CP 15064, CEP 91501-970, Porto Alegre, RS, Brazil
F. Combes
Affiliation:
LERMA – Observatoire de Paris, 61 Av. de l'Observatoire, F-75014 Paris, France
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Using N-body numerical simulations, we investigate the stability of a nuclear disk of a few pc characteristic radius, around a supermassive black hole (SBH), and embedded in a galactic bulge. We find that with an SBH of a suitable range of mass, placed at its center, the nuclear disk is subject to one-armed (m=1) natural instabilities. We propose a feedback cycle for this mode, based on waves between corotation and OLR, and where the “indirect term”, and the massive bulge play a fundamental role. Nuclear disks formed from accreted gas could be the precursors of this type of structure and may be common in central regions of galaxies. Density waves could be an efficient mechanism of fueling the gas in the central few tens of parsecs in galaxies.To search for other articles by the author(s) go to: http://adsabs.harvard.edu/abstract_service.html

Type
POSTERS
Copyright
© 2004 International Astronomical Union