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An inflationary disk phase of protoplanetary disks

Presentation #321.01 in the session Asteroids: Origins (Oral Presentation)

Published onOct 23, 2023
An inflationary disk phase of protoplanetary disks

Understanding planetesimal formation is an essential first step to understanding planet formation. The distribution of these first solid bodies drives the locations where planetary embryos, which eventually form fully-fledged planets, grow. [1, 2].

When considering the Solar System, a proposed model for disk formation and evolution must meet at least the following three criteria:

  1. It must produce an extended dust disk (i.e., at least 45 au [3]).

  2. In at least two distinct locations in the disk, the dust/gas ratio must be able to increase sufficiently to produce planetesimals and explain the early formation of the parent bodies of non-carbonaceous and carbonaceous iron meteorites [e.g., 4].

  3. Dust particles, which have condensed at high temperatures (i.e., calcium–aluminium-rich inclusions, CAIs), must be transported to the outer disk [5].

Recent 1D disk models tracking the evolution of disk and planetesimal formation can satisfy criteria 2 & 3 but not 1 [e.g., 6-9]. Their disks extend only slightly beyond the water snowline (~5 au) because of the rapid dust growth beyond the snowline and subsequent drift back towards the proto-star due to aerodynamic drag in the tangential direction [e.g., 10, 11]. Models where material falls into the disk at large distances [e.g., 12] naturally satisfy criteria 1 and, in some cases, 2 but not 3. We have thus performed an extensive parameter study to find scenarios of disk formation and evolution that satisfy all three conditions.

We will show that an initial rapid expansion — forming an inflationary disk stage — can satisfy all three conditions. Such a disk stage can be induced, e.g., by a high initial viscosity of the gas disk or a short infall timescale of material from the collapsing molecular cloud onto the disk.

Refreneces: [1] Chambers 2001, Icarus, 152, 205 [2] Walsh et al. 2011, Nature, 475, 206 [3] Nesvorný, Vokrouhlický, & Fraser 2022, AJ, 163, 137 [4] Kruijer, T. et al. 2017, Proceoemy of Science, 114, 6712 [5] Zolensky et al. 2006, Science 314, 1735 [6] Drążkowska et al. 2016, A&A, 594, A105 [7] Drążkowska & Dullemond 2018, A&A, 614, A62 [8] Charnoz et al. 2019, A&A, 627, A50 [9] Morbidelli et al. 2022, Nature Astronomy, 6, 72 [10] Takeuchi & Lin 2002, ApJ, 581, 1344 [11] Takeuchi & Lin 2005, ApJ, 623, 482 [12] Hueso & Guillot 2005, A&A, 442, 703

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