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Advection-dominated accretion: A self-similar solution
Narayan, Ramesh; Yi, Insu
AA(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, US), AB(Harvard-Smithsonian Center for Astrophysics, Cambridge, MA, US)
The Astrophysical Journal, vol. 428, no. 1, pt. 1, p. L13-L16 (ApJL Homepage)
Publication Date:
NASA/STI Keywords:
Accretion Disks, Advection, Astronomical Models, Black Holes (Astronomy), Cooling Flows (Astrophysics), Stellar Mass Accretion, Viscous Flow, Hydrodynamics, Rotating Disks, Two Dimensional Flow
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We consider viscous rotating accretion flows in which most of the viscously dissipated energy is stored as entropy rather than being radiated. Such advection-dominated flows may occur when the optical depth is either very small or very large. We obtain a family of self-similar solutions where the temperature of the accreting gas is nearly virial and the flow is quasi-spherical. The gas rotates at much less than the Keplerian angular velocity; therefore, the central stars in such flows will cease to spin up long before they reach the break-up limit. Further, the Bernoulli parameter is positive, implying that advection-dominated flows are susceptible to producing outflows. Convection is likely in many of these flows and, if present, will tend to enhance the above effects. We suggest that advection-dominated accretion may provide an explanation for the slow spin rates of accreting stars and the widespread occurence of outflows and jets in accreting systems.

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