The shape of the inner rim in proto-planetary disks

By Andrea Isella, A. Natta. 2005

168 citations recorded by the source corpus.

We discuss the properties of the inner puffed-up rim that forms in circumstellar disks when dust evaporates. We argue that the rim shape is controlled by a fundamental property of circumstellar disks, namely their very large vertical density gradient, through the dependence of grain evaporation temperature on gas density. Numerical models show that the bright side of the rim is naturally curved, rather than vertical as expected when a constant evaporation temperature is assumed. The rim emits most of its radiation in the near and mid-IR, and provides a simple explanation to the observed values of the near-IR excess (the “ 3 μ m bump” of Herbig Ae stars). We have computed synthetic images of the curved rim. Face-on rims are seen as bright, centrally symmetric rings on the sky; increasing the inclination, the rim takes an elliptical shape, with one side brighter than the other.

Subfields: Astronomy and Astrophysics

View Paper: https://www.semanticscholar.org/paper/498bbeb5c8cece5d5bcbcf9b11a49eb354886287

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In Astronomy and Astrophysics

Citations in the corpus

Radiation thermo-chemical models of protoplanetary disks I. Hydrostatic disk structure and inner rim (2009, background): “In contrast, Isella & Natta (2005) investigated the effect of pressure-dependent sublimation of refractory grains on the shape of the inner rim.”
Accretion Rates in Herbig Ae stars (2006, background): “…crucial for understanding the disk geometry, in particular the nature of the disk inner rim (e.g., Natta et al. 2001; Dullemond et al. 2001; Isella & Natta 2005), which can only form if the accretion rate is lower than a critical value of the order of 10−7 M⊙/yr (Muzerolle et al. 2004).”
STRUCTURE AND EVOLUTION OF PRE-MAIN-SEQUENCE CIRCUMSTELLAR DISKS (2009, background): “At about R = 0.1 AU, the dust sublimates, forming a “puffed-up” inner rim (Isella & Natta 2005) which emits mostly in the near-infrared between 1 and 3 µm (long-short dashed lines).”
Few Skewed Disks Found in First Closure-Phase Survey of Herbig Ae/Be Stars (2006, result): “A “skewed ring” model was developed in order to quantify our results and the observed small closure phases favor inner dust rims which are smoothly curved (e.g., Isella & Natta 2005).”
The Inner Regions of Protoplanetary Disks (2010, methodology): “This was predicted by Isella & Natta (2005) and Vinković (2006) based on 1-”
Millimeter imaging of HD 163296: probing the disk structure and kinematics (2007, background): “The inner disk is characterized by the presence of a puffed-up inner rim located at the dust evaporation radius (Isella and Natta, 2005).”
Disk Surface Density Transitions as Protoplanet Traps (2006, background): “We also stress that at the inner dust puffed-up rims of protoplanetary disks (Isella & Natta 2005), there can be a large radial gradient of the gas temperature, which may be sufficient to trap migrating planets.”
CIRCUMVENTING THE RADIATION PRESSURE BARRIER IN THE FORMATION OF MASSIVE STARS VIA DISK ACCRETION (2010, methodology): “The local evaporation temperature of the dust grains is calculated by using the formula of Isella & Natta (2005) Tevap = gρβ (21) with g = 2000 K, β = 0.0195, and the gas density ρ given in g cm−3.”
THREE-DIMENSIONAL SIMULATION OF MASSIVE STAR FORMATION IN THE DISK ACCRETION SCENARIO (2011, methodology): “For this purpose, we use tabulated dust opacities by Laor & Draine (1993), including 79 frequency bins, and calculate the local evaporation temperature of the dust grains by using the formula of Isella & Natta (2005).”
Fossilized condensation lines in the Solar System protoplanetary disk (2015, background): “However, the vertical isothermal approximation is in many cases a poor proxy for the thermal structure of the disk (see below), so that in reality the condensation ‘‘line” is a curve in ðr; zÞ space, like any other isothermal curve (Isella and Natta, 2005).”
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).”