SINTERING-INDUCED DUST RING FORMATION IN PROTOPLANETARY DISKS: APPLICATION TO THE HL TAU DISK

By S. Okuzumi, M. Momose, S. Sirono, H. Kobayashi, Hidekazu Tanaka. 2015

198 citations recorded by the source corpus.

The latest observation of HL Tau by ALMA revealed spectacular concentric dust rings in its circumstellar disk. We attempt to explain the multiple ring structure as a consequence of aggregate sintering. Sintering is known to reduce the sticking efficiency of dust aggregates and occurs at temperatures slightly below the sublimation point of the constituent material. We present a dust growth model that incorporates sintering and use it to simulate global dust evolution due to sintering, coagulation, fragmentation, and radial inward drift in a modeled HL Tau disk. We show that aggregates consisting of multiple species of volatile ices experience sintering, collisionally disrupt, and pile up at multiple locations slightly outside the snow lines of the volatiles. At wavelengths of 0.87–1.3 mm, these sintering zones appear as bright, optically thick rings with a spectral slope of ≈ 2 , whereas the non-sintering zones appear as darker, optically thinner rings of a spectral slope of ≈ 2.3 –2.5. The observational features of the sintering and non-sintering zones are consistent with those of the major bright and dark rings found in the HL Tau disk, respectively. Radial pileup and vertical settling occur simultaneously if disk turbulence is weak and if monomers constituting the aggregates are ∼ 1 μ m in radius. For the radial gas temperature profile of T = 310 ( r / 1 au ) − 0.57 K , our model perfectly reproduces the brightness temperatures of the optically thick bright rings and reproduces their orbital distances to an accuracy of ≲ 30 % .

Subfields: Astronomy and Astrophysics, Instrumentation

View Paper: https://www.semanticscholar.org/paper/5c52dde90f3db595effd4c300e4c4b4e47929cfe

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Citations in the corpus

Gaps and Rings in an ALMA Survey of Disks in the Taurus Star-forming Region (2018, background): “…regions, also referred to as condensation fronts or ice lines, are locations where dust opacities and collisional growth/fragmentation are expected to change, producing features like gaps and rings seen in dust images (e.g., HL Tau; Banzatti et al. 2015; Zhang et al. 2015; Okuzumi et al. 2016).”
RINGED SUBSTRUCTURE AND A GAP AT 1 au IN THE NEAREST PROTOPLANETARY DISK (2016, background): “The net result is a sequence of traffic jams that locally enhance the solid densities and would appear as bright continuum rings at a set of specific temperatures (Okuzumi et al. 2015).”
The Disk Substructures at High Angular Resolution Project (DSHARP). II. Characteristics of Annular Substructures (2018, background): “Snowlines Previously detected substructures in the HL Tau, TW Hya, and HD 163296 disks have been hypothesized to be due to volatile freezeout altering the coagulation and fragmentation properties of dust grains (e.g., Zhang et al. 2015; Okuzumi et al. 2016; Pinilla et al. 2017).”
Dust Evolution and the Formation of Planetesimals (2016, background): “Other proposed explanations include pressure bumps formed due to magnetised turbulence (Johansen et al. 2009; Dittrich et al. 2013; Flock et al. 2015) or condensation fronts (Cuzzi & Zahnle 2004; Ros & Johansen 2013; Zhang et al. 2015; Okuzumi et al. 2015).”
Three Radial Gaps in the Disk of TW Hydrae Imaged with SPHERE (2016, background): “Dust evolution (Birnstiel et al. 2015), increased coagulation efficiency after ice condensation fronts (Zhang et al. 2015), and a sintering-induced change of agglomeration state (Okuzumi et al. 2016) may all lead to ringed structures in disks.”
ALMA continuum observations of the protoplanetary disk AS 209. Evidence of multiple gaps opened by a single planet (2017, background): “…formation of gaps and rings in disks can be due to several mechanisms such as: planet formation (e.g., Papaloizou & Lin 1984); magneto-rotational instability (Flock et al. 2015); condensation fronts (Zhang et al. 2015); dust sintering (Okuzumi et al. 2016); photoevaporation (Ercolano et al. 2017).”
The Disk Substructures at High Angular Resolution Project (DSHARP). VII. The Planet–Disk Interactions Interpretation (2018, background): “…young planets, we want to point out that there are many other possible mechanisms to produce gaps and rings, such as ice lines (Zhang et al. 2015; Okuzumi et al. 2016), the dead zone transition (Pinilla et al. 2016), MHD zonal flows (Flock et al. 2015; Ruge et al. 2016), the secular GI…”
A Kinematical Detection of Two Embedded Jupiter-mass Planets in HD 163296 (2018, background): “…(Bae, et al. 2017; Fedele et al. 2018), while grain growth around ice lines (Zhang et al. 2015) and the shepherding of dust by (magneto-)hydrodynamic instabilities have also been shown to produce ring like structure in the continuum (Flock et al. 2015; Birnstiel et al. 2015; Okuzumi et al. 2016).”
Planetesimal formation near the snowline: in or out? (2017, background): “On the other hand, according to Sirono (2011) and Okuzumi et al. (2016), the fragmentation threshold velocity for icy pebbles near the snowline is reduced due to sintering.”
ALMA unveils rings and gaps in the protoplanetary system HD 169142: signatures of two giant protoplanets (2017, background): “…instability that creates dead-zones (Flock et al. 2015), dust grain growth corresponding to condensation fronts (Zhang et al. 2015), fusing of dust grains at temperatures below the sublimation point (dust sintering, Okuzumi et al. 2016), and photoevaporation (Ercolano et al. 2017).”