Probing dust grain evolution in IM Lupi's circumstellar disc. Multi-wavelength observations and mo

By C. Pinte, D. Padgett, F. Ménard, K. Stapelfeldt, G. Schneider, J. Olofsson, O. Panic, J. Augereau, G. Duchêne, J. Krist and 12 more. 2008

140 citations recorded by the source corpus.

Aims. We present a panchromatic study, involving a multiple technique approach, of the circumstellar disc surrounding the T Tauri star IM Lupi (Sz 82). Methods. We have undertaken a comprehensive observational study of IM Lupi using photometry, spectroscopy, millimetre interferometry and multi-wavelength imaging. For the first time, the disc is resolved from optical and near-infrared wavelengths in scattered light, to the millimetre regime in thermal emission. Our data-set, in conjunction with existing photometric data, provides an extensive coverage of the spectral energy distribution, including a detailed spectrum of the silicate emission bands. We have performed a simultaneous modelling of the various observations, using the radiative transfer code MCFOST, and analysed a grid of models over a large fraction of the parameter space via Bayesian inference. Results. We have constructed a model that can reproduce all of the observations of the disc. Our analysis illustrates the importance of combining a wide range of observations in order to fully constrain the disc model, with each observation providing a strong constraint only on some aspects of the disc structure and dust content. Quantitative evidence of dust evolution in the disc is obtained: grain growth up to millimetre-sized particles, vertical stratification of dust grains with micrometric grains close to the disc surface and larger grains which have settled towards the disc midplane, and possibly the formation of fluffy aggregates and/or ice mantles around grains.

Subfields: Astronomy and Astrophysics, Insect Science

View Paper: https://www.semanticscholar.org/paper/7a955cdb3d661f5ad2b7fb434c57b8109538800a

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In Astronomy and Astrophysics

In Insect Science

Kecheng Zhang

Citations in the corpus

GLOBAL SIMULATIONS OF PROTOPLANETARY DISKS WITH OHMIC RESISTIVITY AND AMBIPOLAR DIFFUSION (2015, methodology): “…which is in agreement with observational constraints for this value based on sub-mm observations (Andrews et al. 2009), and from multi-wavelength imaging (Pinte et al. 2008).1 The radial power-law exponents for the gas surface density, Σ(R), are −1/2 for our fiducial model, and −3/8 for the…”
Thanatology in protoplanetary discs - The combined influence of Ohmic, Hall, and ambipolar diffusion on dead zones (2014, background): “This could be a problem, since observations have implied that sub-µm grains are present in the upper atmospheres of protoplanetary discs (Pinte et al. 2008).”
DUST AND GAS IN THE DISK OF HL TAURI: SURFACE DENSITY, DUST SETTLING, AND DUST-TO-GAS RATIO (2015, methodology): “We use standard disk parameters to describe the disk structure (e.g. Pinte et al. 2008a; Andrews et al. 2009, see Section 3.1) except for the surface density which shape is let free and is fitted for.”
PROTOPLANETARY DISK STRUCTURES IN OPHIUCHUS (2009, background): “This degeneracy can potentially be alleviated using independent constraints on the vertical structure of the disk, either with multi-transition molecular line data (e.g., Dartois et al. 2003) or high resolution scattered light images (e.g., Pinte et al. 2008).”
THE TW Hya DISK AT 870 μm: COMPARISON OF CO AND DUST RADIAL STRUCTURES (2011, result): “However, Panić et al. (2009) argued that similar modifications to the model structure of the IM Lup disk (see Pinte et al. 2008) were insufficient to account for the much different sizes they measure for its gas and dust emission.”
Molecules with ALMA at Planet-forming Scales (MAPS). I. Program Overview and Highlights (2021, methodology): “It stands out among other Lupus sources due to its disk mass, estimated to be 0.1-0.2 M based on continuum (spectral energy distribution, scattered light images, and resolved millimeter images), and CO multi-isotopologue, multi-line data (Pinte et al. 2008; Cleeves et al. 2016b).”
The Disk Substructures at High Angular Resolution Project (DSHARP). V. Interpreting ALMA Maps of Protoplanetary Disks in Terms of a Dust Model (2018, background): “When observed at millimeter wavelengths, however, we see a disk with small-scale ring and spiral substructure that can only be explained if the geometry of this dust layer is vertically geometrically thin (e.g., Pinte et al. 2008, Huang et al. 2018b).”