Astronomy and Astrophysics – Astrophysics
Scientific paper
1994-03-23
Astrophys.J. 428 (1994) L13
Astronomy and Astrophysics
Astrophysics
7 pages of text, 1 postscript figure, plain TeX, Harvard-Smithsonian Center for Astrophysics Preprint Series No. 3809
Scientific paper
10.1086/187381
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 occurrence of outflows and jets in accreting systems.
Narayan Ramesh
Yi Insu
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