2005/08/25 by T. J. -L. Courvoisier, T. J.-L. Courvoisier, M. Türler +1 · 1 citation
Physics and Astronomy · #Accretion (finance) #Accretion disc #Active galactic nucleus #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Star Formation Studies #Black hole (networking) #Galaxies: Formation, Evolution, Phenomena #Galaxy #Physics #Quasar #Radiation #astro-ph
paper · pdf · doi:10.1051/0004-6361:20040527
Accepted in A+A, 8 pages, 2 figures
arxiv created 2005/08/25 · openalex publication_date 2005/11/25 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
We discuss accretion flows on massive black holes in which different elements of the flow (clumps) have velocities that may differ substantially. We estimate the consequence of collisions between these clumps as they come close to the central object and calculate the resulting radiation. We show that this radiation is similar to that observed in the optical to X-ray spectral domain in Seyfert galaxies and quasars. We also show that the large scale accretion is likely to be clumpy when arriving in the active region and that the clumps keep their identity between collisions.