MG13 - Talk detail

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Abstract

We examine the low angular momentum flow model of Sgr A*, using two-dimensional radiation hydrodynamical calculations based on the parameters of the specific angular momentum and total energy estimated in the recent analyses of stellar wind of nearby stars around Sgr A*. The accretion flow with the plausible parameters is non-stationary and the irregularly oscillatory shock is formed in the inner region of a few tens to a hundred and sixty Schwarzschild radii. Due to the oscillatory shock, the luminosity and the mass outflow rate vary by more than a factor of 2-5 on time scales of an hour to several days. The oscillatory shock is necessarily triggered if the specific angular momentum and the specific energy belong to or are located just nearby in the range of parameters responsible for a stationary centrifugally pressure-supported shock in the inviscid accretion flow. These time variabilities may be relevant to the flare activities of Sgr A*.

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