2001/11/01 by Kelly Holley-Bockelmann, Kelly Holley‐Bockelmann, J. Christopher Mihos +4 · 2 citations
Physics and Astronomy · #Astronomy #Astronomy and Astrophysical Research #Astrophysics #Black Holes and Theoretical Physics #Black hole (networking) #Elliptical galaxy #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Physics #Supermassive black hole #astro-ph
paper · pdf · doi:10.1086/338683
15 pages, 7 figures (1 color). Accepted for publication in ApJ
arxiv created 2001/11/01 · openalex publication_date 2002/03/10 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We use numerical simulations to study the evolution of triaxial elliptical galaxies with central black holes. In contrast to earlier studies which used galaxy models with central density "cores," our galaxies have steep central cusps, as observed in real ellipticals. As a black hole grows in these cuspy triaxial galaxies, the inner regions become rounder owing to chaos induced in the orbital families that populate the model. At larger radii, however, the models maintain their triaxiality, and orbital analyses show that centrophilic orbits there resist stochasticity over many dynamical times. While black hole-induced evolution is strong in the inner regions of these galaxies and reaches out beyond the nominal "sphere of influence" of a black hole, our simulations do not show evidence for a rapid global transformation of the host. The triaxiality of observed elliptical galaxies is therefore not inconsistent with the presence of supermassive black holes at their centers.