Numerical Simulation of Dust Aggregate Collisions. II. Compression and Disruption of Three-Dimensional Aggregates in Head-on Collisions

By K. Wada, Hidekazu Tanaka, Toru Suyama, H. Kimura, Tetsuo Yamamoto. 2008

171 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Ocean Engineering

View Paper: https://www.semanticscholar.org/paper/862d733047603e0989c8731ad858a9d488876522

How researchers see this paper

The researchers whose trusted networks rank it highest, strongest advocate first. Every researcher gets a different order.

In Astronomy and Astrophysics

1. Anders Johansen
2. T. Birnstiel
3. C. Dullemond
4. C. Ormel
5. Michiel Lambrechts
6. H. Klahr
7. M. Fang
8. J. Blum

In Ocean Engineering

1. J. Blum
2. C. Ormel
3. S. Okuzumi
4. Hidekazu Tanaka
5. K. Wada
6. C. Guttler
7. C. Dullemond
8. B. Gundlach

Citations in the corpus

• Gas- and dust evolution in protoplanetary disks (2010, background): “The fragmentation probability is still not well known and subject of both theoretical (Paszun & Dominik 2009; Wada et al. 2008) and experimental research (seeBlum & Wurm 2008; Güttler et al. 2009).”
• 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).”
• ELECTRIC CHARGING OF DUST AGGREGATES AND ITS EFFECT ON DUST COAGULATION IN PROTOPLANETARY DISKS (2009, background): “On the other hand, as shown by recent N-body simulations (Wada et al. 2008), catastrophic fragmentation will take place for relative velocity Δu 30 m s−1.”
• 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.”
• RAPID COAGULATION OF POROUS DUST AGGREGATES OUTSIDE THE SNOW LINE: A PATHWAY TO SUCCESSFUL ICY PLANETESIMAL FORMATION (2012, methodology): “In fact, Equations (12)–(14) are more naturally described in terms of variables in the 2.5-dimensional space, Vf ∝ a5/2, ρ f ∝ N1+2/Vf , and Pf = −dEimp/dVf (see Wada et al. 2008; Suyama et al. 2008).”
• Dust Evolution and the Formation of Planetesimals (2016, background): “These stiffer bounds between monomers might help overcome the radial drift barrier or destructive collisions: Wada et al. (2008) simulated collisions of icy aggregates of sizes of a few micrometers6 and derived a fragmentation threshold velocity of around 50ms−1.”
• A simple model for the evolution of the dust population in protoplanetary disks (2012, background): “It has been suspected that icy particles fragment only at higher velocities due to the ∼10 times higher surface energies (Wada et al. 2008; Gundlach et al. 2011).”
• Fluffy dust forms icy planetesimals by static compression (2013, unknown): “1b (Dominik & Tielens 1997; Wada et al. 2007, 2008, 2009; Suyama et al. 2008, 2012; Paszun & Dominik 2008, 2009; Okuzumi et al. 2012).”
• Planetesimal formation by sweep-up: how the bouncing barrier can be beneficial to growth (2012, background): “…setups and material properties (Blum & Münch 1993; Heißelmann et al. 2007; Langkowski et al. 2008; Kelling & Wurm 2009; Güttler et al. 2010; Weidling et al. 2012), but molecular dynamics simulations show significantly less or no bouncing (Wada et al. 2007, 2008, 2009; Paszun & Dominik 2009).”
• Dust coagulation and fragmentation in molecular clouds. I. How collisions between dust aggregates alter the dust size distribution (2009, background): “Figure 9c presents the results of the standard model in which collisions are restricted to take place head-on, an assumption that is frequently employed in collision studies (e.g., Wada et al. 2008; Suyama et al. 2008).”