MG13 - Talk detail

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Two component advective flows are the most physical accretion disks which arise from theoretical consideration. Here high viscosity matter settles as the Keplerian disk on the equatorial plane, while low viscosity matter having lower angular momentum is accreted above and below this plane. Since viscosity is the determining factor, we investigate the effects of viscous stresses on accretion flows around a non­ rotating black hole by time dependent hydrodynamical calculations, in great detail. As a consequence of angular momentum transfer by viscosity in a two ­dimensional, rotating, axi­symmetric accretion flow, the angular momentum distribution is modified. We show that the centrifugal pressure supported shocks became weaker with the inclusion of viscosity. We also find that as the viscosity is increased, the amount of out flowing matter in the wind is decreased to less than a percentage of the inflow matter. Since the post­shock region acts as a reservoir of hot electrons or the so­ called ‘Compton cloud’, the size of which changes with viscosity, the spectral properties are expected to depend on viscosity very strongly: the harder states are dominated by low­ angular momentum and the low viscosity flow with a significant outflows while the softer states are dominated by the high viscosity Keplerian flow having very little outflows. We include cooling effects and found that a Keplerian disk is produced on the equatorial plane and the flow above and below remains sub­ Keplerian. This gives a complete picture to date, of the formation of a Two component advective flow around a black hole.

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