A HD thermal irradiated wind from outer thin accretion disk in LLAGNs

Evidently, low-luminosity active galactic nuclei LLAGNs comprise of inner advective disk and outer geometrically thin disk. The wind is inevitable in LLAGNs, mainly interpreted indirect way, also the evidences are growing for the presence of wind in outer thin disk. We present a hydrodynamics HD model for wind from outer thin disk where the main driver is the inner disk irradiation (which is parameterized by a number x in hydrostatic equilibrium equation with a slightly unbalancing role). The model works for a low intense irradiation or from a height zₛ in optically thin medium. We solve the model equations in cylindrical coordinate along the z-axis for a given radius r with assuming a tiny vertical speed vz (cₛ sound speed). The sonic point conditions assure an isobaric regime above the sonic height (zᵐᵃˣ), in addition from the height zf ( zᵐᵃˣ) the radial pressure gradient also supports the fluid rotation, and both conjointly assure a wind ejection from the zᵐᵃˣ with fluid speed. The zᵐᵃˣ increases with x, and beyond a large zᵐᵃˣ (say zᵐᵃˣₜ corresponded to maximum x) there is no physical solution. We start the computation from outer radius rₒᵗʰⁱⁿ to inner rᵢₙᵗʰⁱⁿ with Bondi mass accretion rate ṀBondi, to explore the r dependency of mass inflow rate Ṁ and wind properties. We constrain the model by fixing Ṁ at rᵢₙᵗʰⁱⁿ from the observations of NGC 1097, and check the feasibility of model by comparing the energetics with observed bolometric luminosity. The wind is an equatorial with viewing angle $i>85$degree, and capable to generate red-/blue-shifted lines, it would be a general characteristics for LLAGNs.