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tokens: gas is released in the inner region of the disk, a global transonic structure of such a slim disk surrounding a BH is crucial in modeling the observations. In this work, we derive a global solution to a slim accretion disk with outflows accelerated by radiation force of the disk. The calculations can be applied to model the accretion disks surrounding either massive BHs or stellar mass BHs. We describe our model calculations and results in Sections 2 and 3 . The last section contains the discussion of the results. 2. Model A set of equations describing a slim disk with outflows in cylindrical coordinates are summarized in the previous works (see Gu Lu 2007 ; Kato et al. 2008 ). We consider a steady axisymmetric accretion disk in this work, which is described by the momentum equations, energy equation, continuity equation, and the equation of state. The r -component of the momentum equation isAs was done in many previous works, we adopt the pseudo–Newtonian potential,to simulate the gravity of the BH, where M is the BH mass, and is the Schwarzschild radius (Paczyńsky Wiita 1980 ). The continuity equation is We integrate Equation ( 1 ) over z and obtainwhere Equation ( 3 ) is used, Σ is the surface density, Π is the vertically integrated pressure, Ω is the angular velocity of the gas in the disk, and Ω K is the Keplerian angular velocity. The φ -component of the momentum equation iswhere the α -viscosity of t rφ = − αp is adopted. Integrating Equation ( 5 ) over z -direction, we havewhere the velocity of outflow at the disk surface is v H = v z ( H ), as the outflows driven by the radiation force are considered in our model. By integrating Equation ( 3 ) vertically, it becomesThe term 2 ρv H in this equation represents the mass loss rate in outflows from the unit area of the disk surface. If we further integrate Equation ( 7 ) over r -direction, it becomeswhere the integral constant C can be determined with suitable boundary conditions. As the mass loss rate in the outflows from the unit area of the disk surface are , we haveso the mass accretion rate in the disk at radius r isand the total mass loss rate in the outflows driven from the disk region between r and r out is Substituting Equation ( 7 ) into Equation ( 6 ), we haveWe integrate the angular Equation ( 12 ) over r , which leads torespectively, where Equation ( 9 ) is used, is the angular momentum removed by the outflows from the corresponding disk region, is the mass accretion rate swallowed by the BH, and is rate of angular momentum of the accretion gas flowing into the BH ( j in is the specific angular momentum of the accreting gas swallowed by the BH). The vertical integrated equation of state iswhere μ is the mean molecular weight ( μ = 0.62 is used in this work), and T 0 is the temperature at the mid-plane of the disk (see Equations (7.43)–(7.45) in Kato et al. 2008 ). The isothermal sound speed is . The energy equation of the disk iswhere is the gravitational power released