We present new observations of CO J = 2 - 1 emission from the protoplanetary disk around TW Hya. Emission is detected out to 240 au (4 '') and found to exhibit azimuthal variations up to 20% beyond 180 au (3 ''), with the west side of the disk brighter than the east. This asymmetry is interpreted as tracing the shadow previously seen in scattered light. A re-analysis of the multi-epoch observations of the dust shadow in scattered light from Debes et al. suggests that an oscillatory motion would provide a better model of the temporal evolution of the dust shadow rather than orbital motion. Both models predict an angular offset between the dust shadow and the gas shadow of up to similar to 100 degrees. We attribute this offset to the finite rate at which dust grains and gas molecules can exchange heat, dominated by the collisional rate between gas molecules and dust grains, t (coll). The angular offsets derived are equivalent to collisional timescales that range from the near-instantaneous up to t (coll) similar to 10 yr, depending on whether a straight or curved dust shadow, as suggested by Hubble Space Telescope observations reported by Debes et al., is adopted. The inferred range of t (coll) are consistent with those predictions based on representative gas densities, temperatures, gas-to-dust ratios and grain sizes. These results represent the first time empirical constraints can be placed on t (coll).

Gas and Dust Shadows in the TW Hydrae Disk / R. Teague, J. Bae, M. Benisty, S.M. Andrews, S. Facchini, J. Huang, D. Wilner. - In: THE ASTROPHYSICAL JOURNAL. - ISSN 0004-637X. - 930:2(2022 May 01), pp. 144.1-144.9. [10.3847/1538-4357/ac67a3]

Gas and Dust Shadows in the TW Hydrae Disk

S. Facchini;
2022

Abstract

We present new observations of CO J = 2 - 1 emission from the protoplanetary disk around TW Hya. Emission is detected out to 240 au (4 '') and found to exhibit azimuthal variations up to 20% beyond 180 au (3 ''), with the west side of the disk brighter than the east. This asymmetry is interpreted as tracing the shadow previously seen in scattered light. A re-analysis of the multi-epoch observations of the dust shadow in scattered light from Debes et al. suggests that an oscillatory motion would provide a better model of the temporal evolution of the dust shadow rather than orbital motion. Both models predict an angular offset between the dust shadow and the gas shadow of up to similar to 100 degrees. We attribute this offset to the finite rate at which dust grains and gas molecules can exchange heat, dominated by the collisional rate between gas molecules and dust grains, t (coll). The angular offsets derived are equivalent to collisional timescales that range from the near-instantaneous up to t (coll) similar to 10 yr, depending on whether a straight or curved dust shadow, as suggested by Hubble Space Telescope observations reported by Debes et al., is adopted. The inferred range of t (coll) are consistent with those predictions based on representative gas densities, temperatures, gas-to-dust ratios and grain sizes. These results represent the first time empirical constraints can be placed on t (coll).
Settore FIS/05 - Astronomia e Astrofisica
Article (author)
File in questo prodotto:
File Dimensione Formato  
Teague_2022a.pdf

accesso aperto

Tipologia: Publisher's version/PDF
Dimensione 1.4 MB
Formato Adobe PDF
1.4 MB Adobe PDF Visualizza/Apri
Teague_2022a_arxiv.pdf

accesso aperto

Tipologia: Post-print, accepted manuscript ecc. (versione accettata dall'editore)
Dimensione 8.64 MB
Formato Adobe PDF
8.64 MB Adobe PDF Visualizza/Apri
Pubblicazioni consigliate

Caricamento pubblicazioni consigliate

I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.

Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/2434/929483
Citazioni
  • ???jsp.display-item.citation.pmc??? ND
  • Scopus 0
  • ???jsp.display-item.citation.isi??? 1
social impact