Fluffy dust forms icy planetesimals by static compression

By A. Kataoka, Hidekazu Tanaka, S. Okuzumi, K. Wada. 2013

222 citations recorded by the source corpus.

Context: In planetesimal formation theory, several barriers have been proposed, which are bouncing, fragmentation, and radial drift problems. To understand the structure evolution of dust aggregates is a key in the planetesimal formation. Dust grains become fluffy by coagulation in protoplanetary disks. However, once they become fluffy, they are not sufficiently compressed by collisional compression to form compact planetesimals. Aims: We aim to reveal the pathway of the dust structure evolution from dust grains to compact planetesimals. Methods: Using the compressive strength formula, we analytically investigate how fluffy dust aggregates are compressed by static compression due to ram pressure of the disk gas and self gravity of the aggregates in protoplanetary disks. Results: We reveal the pathway of the porosity evolution from dust grains via fluffy aggregates to form planetesimals, circumventing the barriers in planetesimal formation. The aggregates are compressed by the disk gas to the density of 10^{-3} g/cm^3 in coagulation, which is more compact than the case with collisional compression. Then, they are compressed more by self gravity to 10^{-1} g/cm^3 when the radius is 10 km. Although the gas compression decelerate the growth, they grow enough rapidly to avoid the radial drift barrier when the orbital radius is < 6 AU in a typical disk. Conclusions: We propose fluffy dust growth scenario from grains to planetesimals. It enables the icy planetesimal formation in a wide range beyond the snowline in protoplanetary disks. This result proposes a concrete initial condition of planetesimals for the later stages of the planet formation.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/9b99fdb0d494df3fae42336c8904d0e186d746a0

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Citations in the corpus

Concentrating small particles in protoplanetary disks through the streaming instability (2016, background): “One possibility to circumvent this barrier is to increase the collisional crosssection of the particles by collecting porous icy dust aggregates (Kataoka et al. 2013).”
MILLIMETER-WAVE POLARIZATION OF PROTOPLANETARY DISKS DUE TO DUST SCATTERING (2015, background): “This is a good observational test on the planetesimal formation scenario via fluffy dust aggregates (e.g., Kataoka et al. 2013).”
Planetesimal formation starts at the snow line (2017, background): “…that the icy aggregates are significantly more sticky than silicate grains (Wada et al. 2011; Gundlach et al. 2011) and can thus grow to larger sizes before they fragment, or even grow directly to planetesimal sizes if they are sufficiently porous (Okuzumi et al. 2012; Kataoka et al. 2013).”
Forming the cores of giant planets from the radial pebble flux in protoplanetary discs (2014, background): “This prevents continued particle growth by coagulation (Brauer et al. 2008), except possibly in the inner disc with large particle seeding (Windmark et al. 2012) or porous dust aggregates (Kataoka et al. 2013).”
Multiwavelength analysis for interferometric (sub-)mm observations of protoplanetary disks - Radial constraints on the dust properties and the disk structure (2015, background): “…within 1 Myr (see also Laibe 2014) unless it is halted by the occurrence of dust traps (Whipple 1972; Weidenschilling 1977; Klahr & Henning 1997; Pinilla et al. 2012) or a different aerodynamic behavior when the grains are extremely fluffy aggregates (Okuzumi et al. 2012; Kataoka et al. 2013).”
Dust Evolution and the Formation of Planetesimals (2016, background): “This mechanism could thus form relatively compact planetesimals by avoiding the growth barriers via extremely low internal densities, followed by compression via gas drag and self-gravity to reach cometary densities (Kataoka et al. 2013).”
THE MASS AND SIZE DISTRIBUTION OF PLANETESIMALS FORMED BY THE STREAMING INSTABILITY. I. THE ROLE OF SELF-GRAVITY (2015, background): “Whether this is also the case for icy particles is less clear (e.g., Blum & Wurm 2008; Okuzumi et al. 2012; Kataoka et al. 2013; Wada et al. 2013; Krijt et al. 2015; Musiolik et al. 2016).”
Close-in planetesimal formation by pile-up of drifting pebbles (2016, background): “If growth happens even at high impact speeds, for example in the case of very porous dust aggregates, planetesimal formation via direct growth may be possible (Okuzumi et al. 2012; Kataoka et al. 2013).”
THE STICKINESS OF MICROMETER-SIZED WATER-ICE PARTICLES (2014, background): “…threshold of water-ice particles found in our experiments is not in contradiction to the idea that icy planetesimals form by direct sticking of subμm-sized water-ice particles as suggested by Wada et al. (2008, 2009), Suyama et al. (2008, 2012), Okuzumi et al. (2012), and Kataoka et al. (2013).”
Evidence for the formation of comet 67P/Churyumov-Gerasimenko through gravitational collapse of a bound clump of pebbles (2017, background): “If the solid particles are either nonicy or larger than 0.1 µm in size (Kataoka et al. 2013; Lorek et al. 2017), fractal growth comes to a halt, when the impact energy exceeds the restructuring limit (Dominik & Tielens 1997; Blum & Wurm 2000).”