Scattering-induced Intensity Reduction: Large Mass Content with Small Grains in the Inner Region of the TW Hya disk

Ueda, Takahiro; Kataoka, Akimasa; Tsukagoshi, Takashi

doi:10.3847/1538-4357/ab8223

Cited by 52 publications

(57 citation statements)

References 65 publications

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“…This indicates that our model has a too high scattering opacity at millimetre wavelengths and therefore overestimates the total dust optical depth τ ext d within the rings. However, our dust model fits the data because scattering can reduce the observed dust emission as has been shown by Zhu et al (2019), Liu (2019) and Ueda et al (2020). Consequently, the model overestimates the absorption of the back side 12 CO J = 2−1 line emission, resulting in too weak line emission at the location of the dust rings (see Fig.…”

Section: Contribution Of the Back Side Of The Diskmentioning

confidence: 70%

Interpreting high spatial resolution line observations of planet-forming disks with gaps and rings: the case of HD 163296

Rab

Kamp

Dominik

et al. 2020

A&A

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Context. Spatially resolved continuum observations of planet-forming disks show prominent ring and gap structures in their dust distribution. However, the picture from gas observations is much less clear and constraints on the radial gas density structure (i.e. gas gaps) remain rare and uncertain. Aims. We want to investigate the importance of thermo-chemical processes for the interpretation of high-spatial-resolution gas observations of planet-forming disks and their impact on the derived gas properties. Methods. We applied the radiation thermo-chemical disk code PRODIMO (PROtoplanetary DIsk MOdel) to model the dust and gas disk of HD 163296 self-consistently, using the DSHARP (Disk Substructure at High Angular Resolution) gas and dust observations. With this model we investigated the impact of dust gaps and gas gaps on the observables and the derived gas properties, considering chemistry, and heating and cooling processes. Results. We find distinct peaks in the radial line intensity profiles of the CO line data of HD 163296 at the location of the dust gaps. Our model indicates that those peaks are not only a consequence of a gas temperature increase within the gaps but are mainly caused by the absorption of line emission from the back side of the disk by the dust rings. For two of the three prominent dust gaps in HD 163296, we find that thermo-chemical effects are negligible for deriving density gradients via measurements of the rotation velocity. However, for the gap with the highest dust depletion, the temperature gradient can be dominant and needs to be considered to derive accurate gas density profiles. Conclusions. Self-consistent gas and dust thermo-chemical modelling in combination with high-quality observations of multiple molecules are necessary to accurately derive gas gap depths and shapes. This is crucial to determine the origin of gaps and rings in planet-forming disks and to improve the mass estimates of forming planets if they are the cause of the gap.

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Section: Contribution Of the Back Side Of The Diskmentioning

confidence: 70%

Interpreting high spatial resolution line observations of planet-forming disks with gaps and rings: the case of HD 163296

Rab

Kamp

Dominik

et al. 2020

A&A

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“…All of these factors contribute independently and can decrease or increase the reported values within a factor of a few (Ballering & Eisner 2019). Further, given that at the scales of the observed circumstellar disks, dust scattering can decrease the intensity at millimeter wavelengths, which are likely also optically thick, our estimates for the mass of the compact sources should be taken as conservative lower limits (Liu 2019;Ueda et al 2020). The order of magnitude of the lower limits reported here is comparable to other compact (40 au) circumstellar disks in Class I multiple systems observed at high (25 au) resolution, derived in a similar fashion (Takakuwa et al 2017;Alves et al 2019;Cruz-Sáenz de Miera et al 2019).…”

Section: Masses From 3 MM Continuum Emissionmentioning

confidence: 94%

Orbital and Mass Constraints of the Young Binary System IRAS 16293-2422 A

Maureira

Pineda

Segura-Cox

et al. 2020

ApJ

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We present 3 mm ALMA continuum and line observations at resolutions of 6.5 au and 13 au, respectively, toward the Class 0 system IRAS 16293-2422 A. The continuum observations reveal two compact sources toward IRAS 16293-2422 A, coinciding with compact ionized gas emission previously observed at radio wavelengths (A1 and A2), confirming the long-known radio sources as protostellar. The emission toward A2 is resolved and traces a dust disk with an FWHM size of ∼12 au, while the emission toward A1 sets a limit to the FWHM size of the dust disk of ∼4 au. We also detect spatially resolved molecular kinematic tracers near the protostellar disks. Several lines of the J=5−4 rotational transition of HNCO, NH 2 CHO, and t-HCOOH are detected, with which we derived individual line-of-sight velocities. Using these together with the CS (J=2−1), we fit Keplerian profiles toward the individual compact sources and derive masses of the central protostars. The kinematic analysis indicates that A1 and A2 are a bound binary system. Using this new context for the previous 30 yr of Very Large Array observations, we fit orbital parameters to the relative motion between A1 and A2 and find that the combined protostellar mass derived from the orbit is consistent with the masses derived from the gas kinematics. Both estimations indicate masses consistently higher (0.5M 1 M 2  2 M  ) than previous estimations using lowerresolution observations of the gas kinematics. The ALMA high-resolution data provides a unique insight into the gas kinematics and masses of a young deeply embedded bound binary system.

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“…Interestingly, recent multiwavelength studies of the Atacama Large Millimeter/submillimeter Array (ALMA) have shown that Ar in Solids ring and gap structures reside even in the optically thick region (Carrasco-González et al 2019;Macías et al 2021). This implies that the substructures are induced by the temperature variation and/or intensity reduction from scattering (e.g., Liu 2019;Zhu et al 2019;Sierra & Lizano 2020;Ueda et al 2020), not by the density variation. For example, the HL Tau disk has a gap at ∼13 AU at the wavelength where the region is expected to be optically thick (Carrasco-González et al 2019).…”

Section: Implications From Disk Observationsmentioning

confidence: 99%

Jupiter’s “cold” formation in the protosolar disk shadow

Ohno

Ueda

2021

A&A

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Context. Atmospheric compositions offer valuable clues to planetary formation and evolution. Jupiter has been the most well-studied giant planet in terms of its atmosphere; however, the origin of the Jovian atmospheric composition remains a puzzle as the abundances of nitrogen and noble gases as high as those of other elements could only originate from extremely cold environments. Aims. We propose a novel idea for explaining the Jovian atmospheric composition: dust pileup at the H2O snow line casts a shadow and cools the Jupiter orbit so that N2 and noble gases can freeze. Planetesimals or a core formed in the shadowed region can enrich nitrogen and noble gases as much as other elements through their dissolution in the envelope. Methods. We compute the temperature structure of a shadowed protosolar disk with radiative transfer calculations. Then, we investigate the radial volatile distributions and predict the atmospheric composition of Jupiter with condensation calculations. Results. We find that the vicinity of the current Jupiter orbit, approximately 3 − 7 AU, could be as cold as ≲30 K if the small-dust surface density varies by a factor of ≳30 across the H2O snow line. According to previous grain growth simulations, this condition could be achieved by weak disk turbulence if silicate grains are more fragile than icy grains. The shadow can cause the condensation of most volatile substances, namely N2 and Ar. We demonstrate that the dissolution of shadowed solids can explain the elemental abundance patterns of the Jovian atmosphere even if proto-Jupiter was formed near Jupiter’s current orbit. Conclusions. The disk shadow may play a vital role in controlling atmospheric compositions. The effect of the shadow also impacts the interpretation of upcoming observations of exoplanetary atmospheres by JWST.

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Scattering-induced Intensity Reduction: Large Mass Content with Small Grains in the Inner Region of the TW Hya disk

Cited by 52 publications

References 65 publications

Interpreting high spatial resolution line observations of planet-forming disks with gaps and rings: the case of HD 163296

Interpreting high spatial resolution line observations of planet-forming disks with gaps and rings: the case of HD 163296

Orbital and Mass Constraints of the Young Binary System IRAS 16293-2422 A

Jupiter’s “cold” formation in the protosolar disk shadow

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