On the Interferometric Sizes of Young Stellar Objects

By J. Monnier, R. Millan-Gabet. 2002

178 citations recorded by the source corpus.

Long-baseline optical interferometers can now detect and resolve hot dust emission thought to arise at the inner edge of circumstellar disks around young stellar objects (YSOs). We argue that the near-infrared sizes being measured are closely related to the radius at which dust is sublimated by the stellar radiation field. We consider how realistic dust optical properties and gas opacity dramatically affect the predicted location of this dust destruction radius, an exercise routinely done in other contexts but so far neglected in the analysis of near-infrared sizes of YSOs. We also present the accumulated literature of near-infrared YSO sizes in the form of a size-luminosity diagram and compare with theoretical expectations. We find evidence that large (≳1.0 μm) dust grains predominate in the inner disks of T Tauri and Herbig Ae/Be stars, under the assumption that the innermost gaseous disks are optically thin at visible wavelengths.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/61dcce2aa57b48e6b2904295d96ee83e090a1634

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In Astronomy and Astrophysics

1. S. Andrews
2. N. Calvet
3. C. Dullemond
4. D. Wilner
5. A. Natta
6. K. Luhman
7. L. Hartmann
8. Catherine C. Espaillat

In Spectroscopy

1. C. Dullemond
2. K. Luhman
3. A. Natta
4. N. Calvet
5. Andrea Isella
6. Catherine C. Espaillat
7. J. Monnier
8. V. Pi'etu

Citations in the corpus

• Fragmentation of massive protostellar discs (2006, background): “This leads to the disappearance of dust within the infall envelope inside a certain sublimation radius Rs. Monnier & Millan-Gabet (2002) determine Rs ≃ 35(L⋆/10 6L⊙) 1/2 AU by optical interferometry (and note that this value requires the existence of large silicate grains).”
• 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).”
• Accretion disks in luminous young stellar objects (2015, background): “Monnier & Millan-Gabet (2002) demonstrated that the H-band and K-band equivalent ring sizes R (see Sect.”
• UNVEILING THE STRUCTURE OF PRE-TRANSITIONAL DISKS (2010, methodology): “We test wall temperatures between 1000–2000 K, corresponding to the range of dust sublimation temperatures found for a large sample of classical T Tauri stars (CTTS) and Herbig Ae/Be stars (Monnier & Millan-Gabet 2002), and maximum grain sizes of 0.25 µm, 1 µm, and 5 µm.”
• Few Skewed Disks Found in First Closure-Phase Survey of Herbig Ae/Be Stars (2006, methodology): “Interestingly, the NIR ring diameter found here is undersized compared to the normal sizeluminosity relation for Herbig Ae/late Be stars, as also found for some other early Be Herbigs (Monnier & Millan-Gabet 2002; Eisner et al. 2004).”
• Sub-arcsec imaging of the AB Aur molecular disk and envelope at millimeter wavelengths: a non Keplerian disk (2005, background): “Monnier & Millan-Gabet (2002) have shown that in such objects, the very inner dust disk is truncated by sublimation of the dust at temperature around∼ 1500 K.”
• The shape of the inner rim in proto-planetary disks (2005, methodology): “For example, on one side smaller values of Rin can be due to some low-density gas in the inner disk hole, able to absorb the UV continuum from the star (Monnier and Millan-Gabet 2002, Akeson at al.”
• The Inner Regions of Protoplanetary Disks (2010, background): “Monnier & Millan-Gabet (2002) showed that the collective literature data of disk sizes could be best explained by an inner rim of dust surrounding an opticallythin region, giving support to the theoretical ideas of N01 and DDN01.”
• A STELLAR-MASS-DEPENDENT DROP IN PLANET OCCURRENCE RATES (2014, background): “…properties such as disk mass (Mohanty et al. 2013; Andrews et al. 2013), mass accretion rate (e.g., Hartmann et al. 2006; Alcalá et al. 2014), inner disk radius (Monnier & Millan-Gabet 2002; Millan-Gabet et al. 2007), dust evolution (Apai et al. 2005), and disk chemistry (Pascucci et al. 2009).”