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Peer-reviewedCC BY 4.0Monthly Notices of the Royal Astronomical Society

Diverse dust vertical height and settling strength conditions in protoplanetary discs

  • Juanita Antilen
  • Paola Pinilla
  • Dafa Li
  • Marion Villenave
  • Anibal Sierra
  • Yao Liu
  • Myriam Benisty
  • Christian Ginski
Open at sourcePDFDOICite

Abstract

The settling of dust particles plays a critical role in the growth and dynamics of dust grains. Using radiative transfer simulations, we performed detailed modelling of the ALMA continuum substructures for six highly inclined protoplanetary discs to constrain the vertical height of millimetre dust grains and the settling strength. Our modelling results are a very thin millimetre dust disc in T Cha (hdustlt 0.1 au throughout the disc), a vertically extended dust disc in DoAr 25 (hdust of ∼ 4.7 au at 140 au), and tentatively a thin disc in MY Lup (hdustlt 0.5 au at 70 au). From lower resolution observations, we found a very thin disc for PDS 111 (hdustlt 0.1 au throughout the disc) and a more vertically extended millimetre dust disc in V409 Tau (hdust of ∼ 1.3 au at 35 au). We could not measure the vertical height in the asymmetric disc of RY Lup. We also found that the input dust opacities are a source of degeneracy in our models. Our tentative results, assuming the Ricci dust opacities, point to a diverse settling strength in our sample and possible radial variations. We also compared the models that best fit the ALMA data with the SPHERE data to test if they can reproduce the vertical distribution of small dust grains. This comparison suggests that models that reproduce the dust density distribution in the midplane cannot reproduce the distribution of small dust grains in the upper layers, reinforcing the need for more complex models.

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Cite

BibTeXRIS
BibTeX
@article{antilen2026diverse,
  title = {{Diverse dust vertical height and settling strength conditions in protoplanetary discs}},
  author = {Juanita Antilen and Paola Pinilla and Dafa Li and Marion Villenave and Anibal Sierra and Yao Liu and Myriam Benisty and Christian Ginski},
  journal = {Monthly Notices of the Royal Astronomical Society},
  year = {2026},
  month = may,
  doi = {10.1093/mnras/stag882},
  url = {https://hal.science/hal-05771988v1},
  note = {CC BY 4.0},
}
RIS
TY  - JOUR
TI  - Diverse dust vertical height and settling strength conditions in protoplanetary discs
AU  - Juanita Antilen
AU  - Paola Pinilla
AU  - Dafa Li
AU  - Marion Villenave
AU  - Anibal Sierra
AU  - Yao Liu
AU  - Myriam Benisty
AU  - Christian Ginski
PY  - 2026
DA  - 2026/05/21
JO  - Monthly Notices of the Royal Astronomical Society
DO  - 10.1093/mnras/stag882
UR  - https://hal.science/hal-05771988v1
AB  - The settling of dust particles plays a critical role in the growth and dynamics of dust grains. Using radiative transfer simulations, we performed detailed modelling of the ALMA continuum substructures for six highly inclined protoplanetary discs to constrain the vertical height of millimetre dust grains and the settling strength. Our modelling results are a very thin millimetre dust disc in T Cha (h_dustlt 0.1 au throughout the disc), a vertically extended dust disc in DoAr 25 (h_dust of ∼ 4.7 au at 140 au), and tentatively a thin disc in MY Lup (h_dustlt 0.5 au at 70 au). From lower resolution observations, we found a very thin disc for PDS 111 (h_dustlt 0.1 au throughout the disc) and a more vertically extended millimetre dust disc in V409 Tau (h_dust of ∼ 1.3 au at 35 au). We could not measure the vertical height in the asymmetric disc of RY Lup. We also found that the input dust opacities are a source of degeneracy in our models. Our tentative results, assuming the Ricci dust opacities, point to a diverse settling strength in our sample and possible radial variations. We also compared the models that best fit the ALMA data with the SPHERE data to test if they can reproduce the vertical distribution of small dust grains. This comparison suggests that models that reproduce the dust density distribution in the midplane cannot reproduce the distribution of small dust grains in the upper layers, reinforcing the need for more complex models.
SN  - 0035-8711
SN  - 1365-2966
ER  -