Structuring the hot advective accretion flow, as a result interaction of plasma with magnetic field

2014/08/18 by Krasimira Yankova, Yankova, Krasimira, L. Filipov +2
Physics and Astronomy · #Astrophysical Phenomena and Observations #Astrophysics and Star Formation Studies #Atomic and Molecular Physics #FOS: Physical sciences #High Energy Astrophysical Phenomena (astro-ph.HE) #astro-ph.HE

paper · pdf · doi:10.48550/arxiv.1408.4011

23 pages, 5 figures, 40th COSPAR Scientific Assembly Moscow, Russia, 2-10 August 2014

arxiv created 2014/08/18 · openalex publication_date 2014/08/18 · arxiv updated 2014/08/19 · openalex created_date 2016/06/24 · openalex updated_date 2026/07/28

Abstract

We present a magneto-hydrodynamic model developed for investigations of advective non-stationary, asymmetric Keplerian accretion disks in the normal magnetic field. The introduced model allows us to trace the evolution in different fixed moments and to get detailed description of the self-structuring of the disk. We have introduced "meeting coefficients" that define the feedback. It determines the impact from nonlinear effects have over the structure of the flow. We have obtained solutions for the radial structure of the disk for two crucial moments of its evolution.

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