Evolution of protoplanetary disks: Constraints from DM Tauri and GM Aurigae

By Ricardo Hueso, T. Guillot. 2005

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We present a one-dimensional model of the formation and viscous evolution of protoplanetary disks. The formation of the early disk is modeled as the result of the gravitational collapse of an isothermal molecular cloud. The disk’s viscous evolution is integrated according to two parameterizations of turbulence: the classical α representation and a β parameterization, representative of non-linear turbulence driven by the keplerian shear. We apply the model to DM Tau and GM Aur, two classical T-Tauri stars with relatively well-characterized disks, retrieving the evolution of their surface density with time. We perform a systematic Monte-Carlo exploration of the parameter space (i.e. values of the α-β parameters, and of the temperature and rotation rate in the molecular cloud) to find the values that are compatible with the observed disk surface density distribution, star and disk mass, age and present accretion rate. We find that the observations for DM Tau require 0.001 <α< 0. 1o r 2 × 10 −5 <β< 5 × 10 −4 . For GM Aur, we find that the turbulent viscosity is such that 4 × 10 −4 <α< 0.01 or 2 × 10 −6 <β< 8 × 10 −5 .T hese relatively large values show that an efficient turbulent diffusion mechanism is present at distances larger than ∼10 AU. This is to be compared to studies of the variations of accretion rates of T-Tauri stars versus age that mostly probe the inner disks, but also yield values of α ∼ 0.01. We show that the mechanism responsible for turbulent diffusion at large orbital distances most probably cannot be convection because of its suppression at low optical depths.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/0b5212271666092859fb54a1f2b4254bbd2dc7ff

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Citations in the corpus

Gas- and dust evolution in protoplanetary disks (2010, background): “B), Tirr = T⋆ · [ 2 3π (R⋆ r )3 + 1 2 (R⋆ r )2 (Hp r ) ( d ln Hp d ln r − 1 )] 1 4 , (26) with a fixed dlnHp/dlnr = 9/7, following Hueso & Guillot (2005).”
ON THE ROLE OF DISKS IN THE FORMATION OF STELLAR SYSTEMS: A NUMERICAL PARAMETER STUDY OF RAPID ACCRETION (2009, background): “In addition to numerical work, there are a range of semi-analytic models which follow the time evolution of accreting disks (Hueso & Guillot 2005, KMK08).”
PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS. II. EXTENSION TO FAINTER SOURCES (2010, methodology): “…∼90% of the disk mass at the formation epoch (here defined as approximately twice an initial scaling radius, ∼2R1), then the specific angular momentum can be written j ≈ 2× 1020 ( R1 25AU )0.5 (M∗ M⊙ )−1.5(Rcore 0.1 pc )2 cm2 s−1, (2) where Rcore is the core radius (see Hueso & Guillot 2005).”
STRUCTURE AND EVOLUTION OF PRE-MAIN-SEQUENCE CIRCUMSTELLAR DISKS (2009, background): “Differences in disk structure are believed to result from variation in the total angular momenta, masses, chemical compositions and magnetic fields, during the collapse of the parent molecular core (see, e.g., Hueso & Guillot 2005).”
The Non-carbonaceous–Carbonaceous Meteorite Dichotomy (2020, background): “The distance where mass is added to the disk increases with time outwards to several AU (e.g., Hueso and Guillot 2005; Yang and Ciesla 2012), and so different regions of the disk received varying proportions of material infalling at different times.”
Photoevaporation of protoplanetary discs - II. Evolutionary models and observable properties (2006, background): “Despite the presence of holes in their (dust) discs, both GM Aur and DM Tau have large accretion rates (on to the star), of the order of 10−8 M yr−1 (Calvet et al. 2005; Hueso & Guillot 2005).”
Protoplanetary Disks and Their Evolution (2011, methodology): “Numerical models of both magnetic and non-magnetic collapsing molecular cores show disks form rapidly, within∼ 104 yr (Hueso & Guillot 2005; Yorke, Bodenheimer & Laughlin 1993).”
The chemical history of molecules in circumstellar disks - I. Ices (2009, background): “…in the disk,cs,d = √ kTm/µmp (with k the Boltzmann constant,mp the proton mass andµ the mean molecular mass of 2.3 nuclei per hydrogen molecule), is different from the sound speed in the envelope,cs, because the midplane temperature of the disk,Tm, varies as described in Hueso & Guillot (2005).”
PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS (2009, background): “A sequence of sophisticated numerical modeling studies that self-consistently track both the formation and subsequent evolution of disks have suggested that larger values near γ ≈ 1.5 are more appropriate (Vorobyov & Basu 2007; Vorobyov 2008, but see Hueso & Guillot 2005).”
Global Models for the Evolution of Embedded, Accreting Protostellar Disks (2007, background): “…long been recognized (Larson 1984), and our study is preceded by evolutionary calculations which incorporate accretion and self-gravity into one-dimensional (Lin & Pringle 1987, 1990; Nakamoto & Nakagawa 1994, 1995; Hueso & Guillot 2005) and two-dimensional (Vorobyov & Basu 2005, 2006) simulations.”
TIME EVOLUTION OF VISCOUS CIRCUMSTELLAR DISKS DUE TO PHOTOEVAPORATION BY FAR-ULTRAVIOLET, EXTREME-ULTRAVIOLET, AND X-RAY RADIATION FROM THE CENTRAL STAR (2009, methodology): “Our model follows mostly the model of Hueso & Guillot (2005), and was used by us in two earlier publications (Dullemond, Natta & Testi 2006 and Dullemond, Apai & Walch 2006).”
Chemical enrichment of giant planets and discs due to pebble drift (2017, methodology): “To compute the temperature, we follow Birnstiel et al. (2010) and use the model of Hueso & Guillot (2005), which includes viscous heating, irradiation from a central star and external radiation.”
PROSAC: A Submillimeter Array Survey of Low-Mass Protostars. I. Overview of Program: Envelopes, Disks, Outflows, and Hot Cores (2007, background): “This may seem a disparity; in a simple picture of envelope material falling into a circumstellar disk and accreting onto the central protostar, the mass of the disk is expected to increase until the envelope has dissipated (e.g., Nakamoto & Nakagawa 1994; Hueso & Guillot 2005).”
HETEROGENEOUS DISTRIBUTION OF 26Al AT THE BIRTH OF THE SOLAR SYSTEM (2010, background): “The mass and angular momentum transport in the disk as well as the addition of mass to both the Sun and the disk due to infall from the parent molecular cloud were considered (Hueso and Guillot 2005; Yang and Ciesla 2010).”
Dynamics of Protoplanetary Disks (2010, background): “The value of α itself can be constrained by studies of the evolution of the stellar accretion rate (Hartmann et al. 1998), or by detailed studies of individual systems (Hueso & Guillot 2005).”