Advection in Accretion Disk Boundary Layers

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Abstract
Recent numerical simulations of accretion disk boundary layers have shown qualitatively the importance of advected energy in the inner region of the disk. In this short paper we present quantitative results of advective boundary layers in the optically thick regime. Numerical results are obtained for various systems, by means of a one-dimensional time-dependent numerical code. At high accretion mass rates, ≈ 10−4 M☉ yr-1, or low values of the viscosity parameter, α ≈ 0.001-0.01 (characteristic of FU Orionis systems and some symbiotic stars), the optical thickness in the inner part of the disk becomes very large (τ 1). The disk, unable to cool efficiently, becomes geometrically thick (H/r ≈ 0.5). The energy dissipated in the dynamical boundary layer is radiated outward to larger radii and advected into the star. The boundary-layer luminosity is only a fraction of its expected value; the rest of the energy is advected into the star. The fraction of the advected energy is ζ = Ladv/Lacc ≈ 0.1 in symbiotic stars (accretion onto a low-mass main-sequence star) and ζ ≈ 0.2 in FU Ori systems (accretion onto a pre-main sequence star).

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