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R. Misra, R.E. Taam (Northwestern Univ.)
The effect of a possible hydrodynamical winds on the nature of hot accretion disk solutions is studied. For the advection dominated branch, the presence of a wind, reduces the ion temperature while the self-similar solution for the disk structure is maintained. The critical accretion rate (\dot Mcrit) beyond which there are no hot disk solutions, is significantly smaller than that obtained by neglecting a wind from the disk. Global solutions are constructed and it is found that the accretion rate variation with radius is a power-law i.e. (\dot M) \propto r\alpha_i, with \alphai varying from zero to unity depending on the strength of the wind and the viscosity parameter.
Winds are not generated for the radiatively cooled hot disk branch with low accretion rates (\dot M << \dot Mcrit), since the ion temperatures are much less than virial. However, for high accretion rates (\dot M \le \dot Mcrit, winds regulate the accreting flow. In particular, global solutions are obtained, wherein \dot M (r) \approx \dot Mcrit (r). The stability of such a flow is discussed.
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