2009/12/09 by Riccardo Benini, Giovanni Montani, Benini, Riccardo +1
Physics and Astronomy · #Astro and Planetary Science #Astrophysics and Star Formation Studies #FOS: Physical sciences #High Energy Astrophysical Phenomena (astro-ph.HE) #Solar and Space Plasma Dynamics #Solar and Stellar Astrophysics (astro-ph.SR) #astro-ph.HE #astro-ph.SR
paper · pdf · doi:10.48550/arxiv.0912.1721
3 pages, 1 figure, presentation given at the Marcel Grossman Meeting XII, July 12 - 18 2009 (Paris)
arxiv created 2009/12/09 · openalex publication_date 2009/12/09 · arxiv updated 2010/01/07 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We discuss basic features of steady accretion disk morphology around magnetized compact astrophysical objects. A comparison between the standard model of accretion based on visco-resistive MHD and the plasma instabilities, like ballooning modes, triggered by very low value of resistivity, is proposed.