1998/01/27 by Sebastian Heinz, Christopher S. Reynolds, Mitchell C. Begelman · 7 citations
Physics and Astronomy · #Astronomy and Astrophysical Research #Astrophysical Phenomena and Observations #Galaxies: Formation, Evolution, Phenomena #astro-ph
paper · pdf · doi:10.1086/305807
submitted to the ApJ, LaTex 2e, 23 pages, 7 postscript figures
arxiv created 1998/01/27 · openalex publication_date 1998/07/01 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/01
We present a simple model for an evolving radio galaxy as it expands into the hot, X-ray-emitting interstellar medium (ISM) of its host galaxy or similarly into the hot intracluster medium (ICM) of its host cluster. We solve the governing equations numerically on a grid of model parameters in order to present simple analytical tools for X-ray observations of the shocked shell that is pushed out by the cocoon and the associated cavity in the cluster emission. We apply these tools to the well-known example of Perseus A to show that its time-averaged kinetic luminosity probably exceeds 10 46 ergs s -1 , much larger than the estimated current power. We show how future observations can be used to extract useful source parameters such as the average kinetic power and the source age, and discuss detectability of sources at various stages of their lives.