Relativistic Accretion Tori around Schwarzschild Black Holes : Astrophysics and Relativity

概要

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The axisymmetric structures of relativistic accretion tori are calculated taking into account all components of the flow velocity of matter. Angular momentum distributions are approximated by a power law of the form, l_φ=c_φλ^n_φ, where λ_φ is the von Zeipel parameter. The radial velocity of the flow must be subsonic at the inner boundary of any torus, implying the flow is subsonic throughout the whole torus. Otherwise, the matter's velocity exceeds the velocity of light in the region between the event horizon and the inner boundary of any torus. Therefore, accretion tori with subsonic flow are calculated. We investigate the effects of various parameters involved in the basic equations which govern the structure of the accretion tori. We also calculate the required shear stress which reproduces the assumed angular momentum distributions. The radial and the meridional velocities play a minor role in the structure of the tori but play an important role in determining the accretion rate and the angular momentum transport due to shear stress.
理論物理学刊行会の論文
1988-09-25