COLLISIONAL GROWTH CONDITIONS FOR DUST AGGREGATES

By K. Wada, Hidekazu Tanaka, Toru Suyama, H. Kimura, Tetsuo Yamamoto. 2009

227 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Spectroscopy

View Paper: https://www.semanticscholar.org/paper/a6d7d23e963835d31686dca4f5a10598eea92965

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Citations in the corpus

The outcome of protoplanetary dust growth: pebbles, boulders or planetesimals? (2009, background): “This agrees with the molecular-dynamics simulations by Dominik & Tielens (1997) and Wada et al. (2007, 2008, 2009).”
THE STICKINESS OF MICROMETER-SIZED WATER-ICE PARTICLES (2014, background): “Coagulation models (Wada et al. 2007, 2008, 2009; Wettlaufer 2010) assume a higher upper energy limit for sticking of ice particles than for silicates (for the latter, see Poppe et al. 2000), but empirical evidence for this conjecture is scarce.”
A simple model for the evolution of the dust population in protoplanetary disks (2012, background): “Recent numerical studies of Wada et al. (2009) found that the fragmentation velocity for 10 μm sized icy aggregates could be as high as 50 m s−1.”
The primordial nucleus of comet 67P/Churyumov-Gerasimenko (2015, background): “It is thus reasonable to assume that the velocity range for growth as described above can be an order of magnitude higher, or 0.3 <∼ vrel <∼ 30 m s−1 (Wada et al. 2009).”
Ring shaped dust accumulation in transition disks (2012, background): “The fragmentation velocities of the dust grains can be estimated based on laboratory experiments and theoretical work of collisions for silicates and ices (e .g., Blum & Wurm 2008; Schäfer et al. 2007; Wada et al. 2009).”
Planetesimal formation by sweep-up: how the bouncing barrier can be beneficial to growth (2012, methodology): “Progress has also been made with numerical simulations of dust (silica and ice) aggregate collisions using moleculardynamics codes (Wada et al. 2009, 2011) with up to 10,000 monomers corresponding to aggregate sizes of around 100µm.”
Trapping dust particles in the outer regions of protoplanetary disks (2011, background): “Outside the snow-line, the presence of ices affects the material properties, making the fragmentation velocities increase (Schäfer et al. 2007; Wada et al. 2009).”
Gas- and dust evolution in protoplanetary disks (2010, background): “This can influence material properties and increase the fragmentation velocity (seeSchäfer et al. 2007; Wada et al. 2009).”
Fluffy dust forms icy planetesimals by static compression (2013, background): “1b (Dominik & Tielens 1997; Wada et al. 2007, 2008, 2009; Suyama et al. 2008, 2012; Paszun & Dominik 2008, 2009; Okuzumi et al. 2012).”
RAPID COAGULATION OF POROUS DUST AGGREGATES OUTSIDE THE SNOW LINE: A PATHWAY TO SUCCESSFUL ICY PLANETESIMAL FORMATION (2012, background): “For instance,N-body collision experiments by Wada et al. (2009) suggest that aggregates made of 0.1µm sized icy grains do not experience catastrophic disruption at collision velocities up to 35–70 m s−1.”
The great dichotomy of the Solar System: Small terrestrial embryos and massive giant planet cores (2015, background): “er for silicate particles (Guttler, 2009), so it is likely that silicate particles could grow to mm-size relatively easily but not beyond (unlike icy particles which can easily grow to larger sizes; Wada et al., 2009; Ros and Johansen, 2013). For all these reasons, we assume that the silicate partic”