Abstract
We study the interactions between a presumed cool disk and its hot corona in the Galactic Center. If the interactions are dominated by mass evaporation, the resultant evaporation rate is larger than the Bondi accretion rate of 10–5M⊙/yr, thus, the disk should have been depleted since the last star had formed. If the interactions result in hot gas steadily condensing into the disk, a very high mass flow rate is required, which is inconsistent with observations. We conclude that, for standard viscosity, there is no thin disk in the Galactic Center now. For very small viscosity, see [4] for an alternative model.
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Liu, B., Meyer, F., Meyer-Hofmeister, E. Accretion in the Galactic Center: Via a Cool Disk?. In: Merloni, A., Nayakshin, S., Sunyaev, R.A. (eds) Growing Black Holes: Accretion in a Cosmological Context. ESO Astrophysics Symposia. Springer, Berlin, Heidelberg. https://doi.org/10.1007/11403913_39
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DOI: https://doi.org/10.1007/11403913_39
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Publisher Name: Springer, Berlin, Heidelberg
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