The Influence of Hydrodynamical Winds on Hot Accretion Disk Solutions.pdfVIP

Draft version February 1, 2008 A Preprint typeset using L T X style emulateapj v. 26/01/00 E THE INFLUENCE OF HYDRODYNAMICAL WINDS ON HOT ACCRETION DISK SOLUTIONS Ranjeev Misra1 and Ronald E. Taam1 Draft version February 1, 2008 ABSTRACT 1 The effect of a possible hydrodynamical wind on the nature of hot accretion disk solutions is studied. 0 It is found that the advection dominated branch, in the presence of a wind, maintains the self-similar 0 solution for the disk structure with the temperature, θ ∝ 1/r, optical depth τ ∝ rP −1/2 and accretion 2 rate m˙ ∝ rP . Based on global solutions cooling due to wind energy loss and advection are found to be equally important. For a wide range of viscosity and wind parameters, the temperature is about b e one-tenth of the virial value and P ≈ 0.9, independent of the mass accretion rate and radius. F In the context of cooling by unsaturated Comptonization of soft photons, solutions also exist where radiative cooling, advection, and wind cooling are important. In this case, wind regulated solutions are 7 possible. Here, the radial dependence of the critical mass accretion rate above which solutions do not exist is unchanged from those solutions without winds. 1 v The wind/advection dominated solutions are loc