Accretion Disk Boundary Layers in Classical T Tauri Stars

Details Accretion Disk Boundary Layers in Classical T Tauri Stars Accretion Disk Boundary Layers in Classical T Tauri Stars

Jun 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996apj...463..674g&link_type=abstract

Astrophysical Journal v.463, p.674

Astronomy and Astrophysics

Astronomy

9

Accretion, Accretion Disks, Stars: Formation, Stars: Pre-Main-Sequence

Scientific paper

Results of one-dimensional time-dependent calculations of geometrically thin accretion disk boundary layers arc presented for classical T Tauri stars for various values of M* (0.8 and 1.0 Msun), R* (1.6, 2.15, and 4.3 Rsun), and Mdot (5 x 1O-9 -5 x 1O-7 Msun yr-1). The results exhibit a thermal boundary layer ( δthBL ≍ 0.1-0.2R*) much larger than the dynamical one (δdynBL few percent), with characteristic low temperatures (TeffBL ≍ 5-6 ×103 K). In the limit of very low mass accretion rates characteristic of T Tauri systems, the mid-plane temperature in the inner disk drops well below 104 K (a few 103 K at most). A very sharp transition region separates the hot ionized thermal boundary layer region from the cool neutral inner disk. For low values of the viscosity parameter (α ≍ 0.01), the medium is optically thin in the cool inner disk and slightly optically thick in the hot thermal boundary layer. This result explains the absence of optically thick material (the "inner hole") as observed in the central part of circumstellar disks around young stellar objects. For higher values of the viscosity parameter (α ≍ 0.1), the optical depth in the boundary layer region decreases (τ ≍ 1) and its temperature increases slightly, while the inner disk becomes partially ionized and optically more thick.

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