1997/09/30 by David Merritt, Gerald D. Quinlan, Gerald Quinlan · 105 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Black hole (networking) #Brightest cluster galaxy #Elliptical galaxy #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy formation and evolution #Galaxy merger #Interacting galaxy #Lenticular galaxy #Rotational symmetry #astro-ph
paper · pdf · doi:10.1086/305579
published in The Astrophysical Journal 498(2), 625-639 (IOP Publishing) · 27 Latex pages, 9 Postscript figures, uses aastex.sty. Accepted for Publication in The Astrophysical Journal, Nov. 26, 1997
arxiv created 1997/11/28 · openalex publication_date 1998/05/10 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/06
We study the effect of a massive central singularity on the structure of a triaxial galaxy using N -body simulations. Starting from a single initial model, we grow black holes with various final masses M h and at various rates, ranging from impulsive to adiabatic. In all cases, the galaxy achieves a final shape that is nearly spherical at the center and close to axisymmetric throughout. However, the rate of change of the galaxy's shape depends strongly on the ratio M h / M g of black hole mass to galaxy mass. When M h / M g ≲ 0.3%, the galaxy evolves in shape on a timescale that exceeds 10 2 orbital periods, or roughly a galaxy lifetime. When M h / M g ≳ 2.5%, the galaxy becomes axisymmetric in little more than a crossing time. We propose that the rapid evolution toward axisymmetric shapes that occurs when M h / M g ≳ 2.5% provides a negative-feedback mechanism that limits the mass of central black holes by cutting off their supply of fuel.