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We consider viscous rotating accretion flows in which most of the viscouslydissipated energy is stored as entropy rather than being radiated. Suchadvection-dominated flows may occur when the optical depth is either very smallor very large. We obtain a family of self-similar solutions where thetemperature of the accreting gas is nearly virial and the flow isquasi-spherical. The gas rotates at much less than the Keplerian angularvelocity; therefore, the central stars in such flows will cease to spin up longbefore they reach the break-up limit. Further, the Bernoulli parameter ispositive, implying that advection-dominated flows are susceptible to producingoutflows. Convection is likely in many of these flows and, if present, willtend to enhance the above effects. We suggest that advection-dominatedaccretion may provide an explanation for the slow spin rates of accreting starsand the widespread occurrence of outflows and jets in accreting systems.Comment: 7 pages of text, 1 postscript figure, plain TeX, Harvard-Smithsonian  Center for Astrophysics Preprint Series No. 380

Advection-dominated accretion: A self-similar solution