Experiments on Sticking, Restructuring, and Fragmentation of Preplanetary Dust Aggregates

By J. Blum, G. Wurm. 2000

346 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Ocean Engineering

View Paper: https://www.semanticscholar.org/paper/6ee1461d60b04c657b7fa5173f41c51479a7ecc0

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Citations in the corpus

THE STICKINESS OF MICROMETER-SIZED WATER-ICE PARTICLES (2014, background): “The only supporting fact for an enhanced stickiness of water ice with respect to silicates is the at least tenfold higher surface energy of water ice (0.19 J m−2; Gundlach et al. 2011) in comparison to silicates (0.02 J m−2; Blum & Wurm 2000; Gundlach et al. 2011).”
Planetesimal formation near the snowline: in or out? (2017, background): “Although micron-sized grains can quite easily coagulate to mm-sized particles (Dominik & Tielens 1997; Ormel et al. 2007), typical relative velocities quickly become so large that particles fragment or bounce rather than stick (Blum & Wurm 2000; Zsom et al. 2010).”
Dust coagulation and fragmentation in molecular clouds. I. How collisions between dust aggregates alter the dust size distribution (2009, methodology): “Thus, when collisional energies are low enough for aggregate restructuring to be unimportant (experimentally determined to be 5 E roll ; Blum & Wurm 2000) particles are in the hit-and-stick regime.”
The outcome of protoplanetary dust growth: pebbles, boulders or planetesimals? (2009, methodology): “The same collisional outcome (but with compaction of the projectile) was found for collisions of small aggregates (Blum & Wurm 2000, Exp. 4 in Table 1).”
BREEDING SUPER-EARTHS AND BIRTHING SUPER-PUFFS IN TRANSITIONAL DISKS (2015, background): “Grain growth in disks can be fast, especially at the high densities that prevail inside 1 AU (e.g., Blum & Wurm 2000; Windmark et al. 2012).”
Particle Pileups and Planetesimal Formation (2003, background): “Current consensus tells us that the threshold velocity that divides sticking from shattering is 1 m s 1 and that the corresponding maximum particle size generated by particle-particle collisions is 1 cm (Weidenschilling & Cuzzi 1993; Blum & Wurm 2000; Wurm, Blum, & Colwell 2001; Chiang 2004).”
The Physics of Protoplanetesimal Dust Agglomerates. I. Mechanical Properties and Relations to Primitive Bodies in the Solar System (2006, background): “Ballistic impact experiments of fractal dust clusters showa transition from fractal to nonfractal growth when the impact energy exceeds the rolling-friction threshold (Blum & Wurm 2000).”
PARTICLE CLUMPING AND PLANETESIMAL FORMATION DEPEND STRONGLY ON METALLICITY (2009, background): “However, small grains can adhere at speeds less than∼ 1 m s−1 (Blum & Wurm 2000).”
Planetesimal Formation by Gravitational Instability (2002, background): “Measurements of interparticle collisions in microgravity experiments reinforce these intuitive impressions; indeed, micron-sized dust particles disrupt larger aggregates upon collision at relative velocities greater than 1 m s 1 (Blum & Wurm 2000).”
WEAK TURBULENCE IN THE HD 163296 PROTOPLANETARY DISK REVEALED BY ALMA CO OBSERVATIONS (2015, background): “Laboratory measurements find that grains can stick together if they collide at less than ∼1–30 m s−1, depending on the composition of the grain (Blum & Wurm 2000, 2008; Poppe et al. 2000; Gundlach et al. 2011), and enhanced turbulence could easily create relative motions that exceed this threshold.”
The effect of gas drag on the growth of protoplanets. Analytical expressions for the accretion of small bodies in laminar disks (2010, background): “Initially, the (relative) velocities between particles are tiny and this is the reason why dust grains can coagulate due to intermolecular forces (Dominik & Tielens 1997; Blum & Wurm 2000) – an effect much harder to envision in the diffuse interstellar medium or even in molecular clouds.”
Numerical Simulation of Dust Aggregate Collisions. II. Compression and Disruption of Three-Dimensional Aggregates in Head-on Collisions (2008, background): “On the other hand, experimental studies (Poppe et al. 2000; Blum & Wurm 2000; Wurm et al. 2005) suggested that the critical velocity was much higher than that of the present results by an order of magnitude.”
Evidence for the formation of comet 67P/Churyumov-Gerasimenko through gravitational collapse of a bound clump of pebbles (2017, background): “The maximum dynamic yield strength can be estimated following the numerical model by Dominik & Tielens (1997) and the experimental results by Blum & Wurm (2000) and is Y = ρv2mc/2 ≈ 1 Pa, with vmc ≈ 1 m s−1 and ρ ≈ 1 kg m−3 being the impact velocity leading to maximum compaction 1 If we assume that…”
Free collisions in a microgravity many-particle experiment. I. Dust aggregate sticking at low velocities (2011, background): “For the initially micrometer-sized dust grains, the collision velocities are small enough to let them stick to each other and form larger, fractal dust aggregates (Wurm and Blum, 1998; Blum et al., 2000; Blum and Wurm, 2000; Krause and Blum, 2004).”
Gravoturbulent Formation of Planetesimals (2005, background): “For relative speeds above a certain threshold, the bodies are likely to break up when they collide rather than to stick (Chokshi et al. 1993; Blum & Wurm 2000).”