Accretion Disks around Young Objects. I. The Detailed Vertical Structure

Abstract

We discuss the properties of an accretion disk around a star with parameters typical of classical T Tauri stars (CTTS), and with the average accretion rate for these disks. The disk is assumed steady and geometrically thin. The turbulent viscosity coefficient is expressed using the alpha prescription and the main heating mechanisms considered are viscous dissipation and irradiation by the central star. The energy is transported by radiation, turbulent conduction and convection. We find that irradiation from the central star is the main heating agent of the disk, except in the innermost regions, R less than 2 AU. The irradiation increases the temperature of the outer disk relative to the purely viscous case. As a consequence, the outer disk (R larger than 5 AU) becomes less dense, optically thin and almost vertically isothermal, with a temperature distribution T proportional to R^{-1/2}. The decrease in surface density at the outer disk, decreases the disk mass by a factor of 4 respect to a purely viscous case. In addition, irradiation tends to make the outer disk regions stable against gravitational instabilities.

41 pages, 14 postscript figures, LaTeX, accepted by ApJ

References in corpus (1)

• Spectral Energy Distributions of T Tauri Stars With Passive Circumstellar Disks

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• The 12CO Gas Structures of Protoplanetary Disks in the Upper Scorpius Region
• Constrained Evolution of a Radially Magnetized Protoplanetary Disk: Implications for Planetary Migration
• Circumplanetary disk ices II. Composition
• Infrared Variability from Circumbinary Disc Temperature Modulations
• Influence of Ohmic and ambipolar heating on thermal structure of accretion discs
• Photophoretic Levitation and Trapping of Dust in the Inner Regions of Protoplanetary Disks
• Observable scattered light features from inclined and non-inclined planets embedded in protoplanetary discs
• Planet Formation by Gas-Assisted Accretion of Small Solids
• A near-infrared, optical and ultraviolet polarimetric and timing investigation of complex equatorial dusty structures
• Dust photophoretic transport around a T Tauri star: Implications for comets composition
• The Impact of Silicate Grain Coagulation on Millimeter Emission from Massive Protostellar Disks
• On the Efficacy of Ocean Formation with a Primordial Hydrogen Atmosphere
• A broken debris cascade as a possible source of hot dust emission in transitioning planet-forming disks
• Thermally driven spontaneous dust accumulation in the inner regions of protoplanetary disks
• Measuring Dust Masses of Protoplanetary Disks in Serpens and L1641/L1647 with ALMA
• Hidden power of near-infrared data for the study of young clusters: Illustrative case of RCW 38
• Note on the "Dead Zone" in Layered Accretion Models
• Vorticity Budget of Weak Thermal Convection in Keplerian disks
• Molecular Line Emission from Accretion Disks Around YSOs
• Statistical analysis of molecular line emission from T Tauri disk models
• Modeling Molecular-Line Emission from Circumstellar Disks
• CO Line Emission Surfaces and Vertical Structure in Mid-Inclination Protoplanetary Disks
• The dispersal of protoplanetary discs -- III: Influence of stellar mass on disc photoevaporation
• Protoplanetary disk formation from the collapse of a prestellar core