2005/09/30 by E. Vitanza, V. Teresi, D. Molteni +1
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics and Star Formation Studies #Galaxies: Formation, Evolution, Phenomena #astro-ph
paper · pdf · doi:10.1086/502711
published as Astrophys.J.643:222-225,2006 · 11 pages, 6 figures, accepted for publication in The Astrophysical Journal
arxiv created 2006/01/27 · openalex publication_date 2006/05/18 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/31
We present a simple physical model of the central source emission in the M87 galaxy. It is well known that the observed X-ray luminosity from this galactic nucleus is much lower than the predicted one, if a standard radiative efficiency is assumed. Up to now the main model invoked to explain such a luminosity was the ADAF (advection-dominated accretion flow) model. Our approach supposes only a simple axisymmetric adiabatic accretion with a low angular momentum together with the bremsstrahlung emission process in the accreting gas. With no other special hypothesis on the dynamics of the system, this model agrees well enough with the luminosity value measured by Chandra .