Passive Irradiated Circumstellar Disks with an Inner Hole

By C. Dullemond, C. Dominik, A. Natta. 2001

620 citations recorded by the source corpus.

A model for irradiated dust disks around Herbig Ae stars is proposed. The model is based on the flaring disk model given by Chiang and Goldreich in 1997, but with the central regions of the disk removed. The inner rim of the disk is puffed up and is much hotter than the rest of the disk because it is directly exposed to the stellar flux. If located at the dust evaporation radius, its reemitted flux produces a conspicuous bump in the spectral energy distribution (SED) that peaks at 2-3 μm. We propose that this emission is the explanation for the near-infrared bump observed in the SEDs of Herbig Ae stars. We study for which stellar parameters this bump would be observable and find that it is the case for Herbig Ae stellar parameters but not for T Tauri stars, confirming what is found from the observations. We also study the effects of the shadow cast by the inner rim over the rest of the flaring disk. The shadowed region can be quite large, and under some circumstances the entire disk may lie in the shadow. This shadowed region will be much cooler than an unshadowed flaring disk, since its only heating sources are radial radiative diffusion and possible indirect sources of irradiation. Under certain special circumstances the shadowing effect can suppress, or even completely eliminate, the 10 μm emission feature from the spectrum, which might explain the anomalous SEDs of some isolated Herbig Ae stars in the recent sample of Meeus and colleagues. At much larger radii the disk emerges from the shadow and continues as a flaring disk toward the outer edge. The emission from the inner rim contributes significantly to the irradiation of this flaring disk. The complete semianalytical model, including structure of the inner edge, the shadowed region, and the flared outer part, is described in detail in this paper, and we show examples of the general behavior of the model for varying parameters.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/a8e1352b142e476a52cafe6fc51e4ab2e267c511

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

In Instrumentation

Citations in the corpus

ISO Spectroscopy of Gas and Dust: From Molecular Clouds to Protoplanetary Disks (2004, background): “Natta et al. (2001) and Dullemond et al. (2001) (see also Dominik et al. 2003) propose a slight modification, in which the inner disk is truncated at the dust sublimation temperature of ∼1400 K at ∼0.5 AU, resulting in a sharp rim exposed to intense radiation and producing most of the near-infrared…”
Interpreting Spectral Energy Distributions from Young Stellar Objects. I. A Grid of 200,000 YSO Model SEDs (2006, background): “…infalling envelope (Ulrich 1976; Terebey et al. 1984), bipolar cavities (Whitney & Hartmann 1993; Whitney et al. 2003a) and a flared accretion disk (Shakura & Sunyaev 1973; Pringle 1981; Kenyon & Hartmann 1987; Chiang & Goldreich 1997; D’Alessio et al. 1998; Dullemond et al. 2001).”
Dust Growth and Settling in Protoplanetary Disks and Disk Spectral Energy Distributions. I. Laminar Disks (2005, background): “…s(Ts) R R 2 T 4 : ðA5Þ The temperature of the disk interior Ti is given by T 4i ¼ 1 2 sin R R 2 T 4 1 exp ½ 2 P; i (Ts) 1 exp ½ 2 P; i (Ti) : ðA6Þ In equations (A5) and (A6), we doubled the left-hand sides, assuming that the entire star is visible from the surface layer (Dullemond et al. 2001).”
[O I] 6300 Å emission in Herbig Ae/Be systems: Signature of Keplerian rotation (2005, methodology): “The puffed-up inner rim in the Dullemond et al. (2001) model naturally explains this excess.”
Optical interferometry in astronomy (2003, background): “A few theorists are incorporating these results into their models, and I recommend the papers of Natta et al. (2001) and Dullemond et al. (2001) for further discussion.”
c2d Spitzer IRS Spectra of Disks around T Tauri Stars. I. Silicate Emission and Grain Growth (2005, methodology): “…the relative contribution of grains from different radii to the 10 and 20 m features, we perform an exercise using a simple two-layer model (CGPLUS; Dullemond et al. 2001; Chiang & Goldreich 1997) to calculate the cumulative disk flux as a function of radius at 10 and 20 m for a typical TT. Figure…”
From molecular cores to planet-forming disks: An SIRTF legacy program (2003, methodology): “…cores and circumstellar disks will be available to help identify the nature of cataloged sources.18 Simple analysis programs for modeling SEDs from disks are being developed for our team based on the formalism by Dullemond et al. (2001) and will be made available through the c2d Web site.”
Resolving the inner dust disks surrounding LkCa 15 and MWC 480 at mm wavelengths (2006, background): “This can be qualitatively understood in Fig.5 in Dullemond et al. (2001), where a change in the slopep of 1 on the dust surface density does not significantly affect the SED (by less than∼ 20 %), which is therefore difficult to disentangle from the other physical effects on real data.”
Mid-infrared sizes of circumstellar disks around Herbig Ae/Be stars measured with MIDI on the VLTI (2004, methodology): “A physical description of the qualitative picture drawn by Meeus et al. (2001) has been given recently in a series of papers by Dullemond et al. (2001) (hereafter DDN), Dullemond (2002) and Dominik et al. (2003).”
PIONIER: a 4-telescope visitor instrument at VLTI (2011, background): “The concept of “puffed-up” inner rim has been introduced (Dullemond et al. 2001; Isella & Natta 2005).”
Probing the structure of protoplanetary disks: a comparative study of DM Tau, LkCa 15, and MWC 480 (2007, background): “Differences between TTauri and Herbig Ae disks are observed in the very inner disk, very close to the star (Dullemond et al. 2001; Monnier & Millan-Gabet 2002).”
Few Skewed Disks Found in First Closure-Phase Survey of Herbig Ae/Be Stars (2006, methodology): “The main achievement of Dullemond et al. (2001) was to couple the radiative transfer to a (vertical) hydrostatic disk structure, finding a physically self-consistent height for the inner rim and the outer disk flaring (which match on to traditional flared disk models, e.g. Chiang & Goldreich 1997).”
Dust grain growth in ρ-Ophiuchi protoplanetary disks (2010, methodology): “In order to constrain the dust properties in the disk outer regions we fitted the sub-mm/mm SED with two-layer (i.e. disk surface and midplane) models of flared disks heated by the radiation of the central star (Chiang & Goldreich 1997; Dullemond et al. 2001).”
Survival of molecular gas in cavities of transition disks - I. CO (2013, background): “Within the dust sublimation radius Rsubl ∼ 0.07√L∗/L AU (assuming a dust sublimation temperature of ∼1500 K; Dullemond et al. 2001), both dust and gas surface density are set to zero.”
A 10 μm spectroscopic survey of Herbig Ae star disks: Grain growth and crystallization (2005, background): “The observed SEDs of these HAe stars can very well be explained with models for gas-rich, passively heated disks in hydrostatic equilibrium and a puffed-up inner rim (Dullemond et al. 2001).”
The Disk Substructures at High Angular Resolution Project (DSHARP). II. Characteristics of Annular Substructures (2018, background): “D’Alessio et al. 1998; Dullemond et al. 2001): Tmid(r) = ( ϕL∗ 8πr2σSB )0.25 , (3) where σSB is the Stefan-Boltzmann constant, L∗ is the stellar luminosity (taken from Table 1 of Andrews et al. (2018b)), and ϕ is the flaring angle.”