The Inner Regions of Protoplanetary Disks

By C. Dullemond, J. Monnier. 2010

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To understand how planetary systems form in the dusty disks around premain-sequence stars, a detailed knowledge of the structure and evolution of these disks is required. Although this is reasonably well understood for the regions of the disk beyond about 1 AU, the structure of these disks inward of 1 AU remains a puzzle. This is partly because it is very difficult to spatially resolve these regions with current telescopes. But it is also because the physics of this region, where the disk becomes so hot that the dust starts to evaporate, is poorly understood. With infrared interferometry it has become possible in recent years to directly spatially resolve the inner 1 AU of protoplanetary disks, albeit in a somewhat limited way. These observations have partly confirmed current models of these regions, but also posed new questions and puzzles. Moreover, it has turned out that the numerical modeling of these regions is extremely challenging. In this review, we give a rough overview of the history and recent developments in this exciting field of astrophysics.

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/f831f2c4f85ff7b83e184e9f511df601343dd4bb

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Citations in the corpus

ALMA Survey of Lupus Protoplanetary Disks. II. Gas Disk Radii (2018, background): “16πσSBr2 )1/4 , (6) where L? is the stellar luminosity and σSB is the StefanBoltzmann constant (e.g., Dullemond & Monnier 2010).”
The warm gas atmosphere of the HD 100546 disk seen by Herschel - Evidence of a gas-rich, carbon-poor atmosphere? (2012, background): “At an important phase of a young low-mass star’s life, the natal envelope has dispersed, but the star is still surrounded by an optically thick protoplanetary disk, which is thought to be the location of planet formation (see Dullemond & Monnier 2010; Armitage 2010, for recent reviews).”
Planet-Disk Interaction and Orbital Evolution (2012, background): “The structure and dynamics of these disks are clearly relevant for understanding planet formation, and we refer the interested reader to three recent reviews that discuss the theory and observations of protoplanetary disks (Dullemond & Monnier, 2010; Armitage, 2011; Williams & Cieza, 2011).”
Protoplanetary Disks and Their Evolution (2011, background): “There are also several related reviews that have been recently written for this series including the inner disk (Dullemond & Monnier 2010), debris disks (Wyatt 2008), and dynamical processes (Armitage 2010).”
Accretion disks in luminous young stellar objects (2015, background): “A comprehensive discussion of the physics and the problems of the disk inner rim of HAeBe stars and an overview of the advances achieved during the first decade of this century can be found in Dullemond & Monnier (2010).”
Our astrochemical heritage (2012, background): “14 Schematic structure of a ”naked” protoplanetary disk, adapted from [324], [139], [395], [138] and [37].”
The minimum-mass extrasolar nebula: in situ formation of close-in super-Earths (2012, background): “Near-infrared interferometric measurements indicate that dust-lines expand with increasing stellar luminosity, from 0.05–0.1 AU in the case of T Tauri stars, to 0.1–0.5 AU for Herbig Ae stars, to 0.5–10 AU for Herbig Be stars (see Figure 7 of the review by Dullemond & Monnier 2010).”
Accretion onto Pre-Main-Sequence Stars (2016, methodology): “In any case, a truncation radius near or inside corotation is consistent with the structure of the inner disk (see the review by Dullemond & Monnier 2010), including the inner radius of CO emission (Najita et al. 2003, Salyk et al. 2011).”
Astrochemistry and compositions of planetary systems (2020, background): “…formation, infalling material is further subject to irradiation (Visser et al. 2009) and accretion shocks (Neufeld and Hollenbach 1994; Visser and Dullemond 2010; Aota et al. 2015; Miura et al. 2017), which may also alter the chemical composition of material that accretes during later, less…”