Growth of planetesimals by impacts at ∼25 m/s

By G. Wurm, G. Paraskov, O. Krauss. 2005

138 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Geophysics

View Paper: https://www.semanticscholar.org/paper/4ab1c368dc4931d7a08496b98e972310232d7ea7

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Citations in the corpus

Rubble Pile Asteroids (2018, background): “Furthermore models of grain growth confront other barriers to growth whereby small mm-sized grains may simply bounce or fragment instead of sticking, effectively limiting the maximum size of simple growth at cm-sizes (Zsom et al. 2010, Wurm et al. 2005, Blum and Wurm 2008, Johansen et al. 2015).”
The outcome of protoplanetary dust growth: pebbles, boulders or planetesimals? (2009, background): “4 in Paraskov et al. 2007) are consistent with Δm mp = 15 20 ( v 100 cm s−1 ) , (38) which agrees with non-zero-gravity experiments of Wurm et al. (2005a), who estimated a mass loss of 10 projectile masses for velocities of more than 1650 cm s−1.”
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.”
The Physics of Protoplanetesimal Dust Agglomerates. I. Mechanical Properties and Relations to Primitive Bodies in the Solar System (2006, background): “An increased mass density can also influence the outcome of a collision between dust aggregates: very fluffy aggregates are more likely to stick to one another in lowvelocity collisions than compacted dusty bodies (Wurm et al. 2005).”
Dust Evolution and the Formation of Planetesimals (2016, unknown): “This type of collisional outcome was first seen in laboratory experiments by Wurm et al. (2005) and subsequently in Paraskov et al. (2007), Teiser & Wurm (2009) as well as in Kothe et al. (2010).”
Asteroids Were Born Big (2009, background): “Current theories predict the destruction of the meter-sized objects at these predicted speeds (Wurm et al., 2005).”
Ice Condensation as a Planet Formation Mechanism (2013, background): “For silicate particles growth via collisions involving equal-sized particles is very difficult beyond millimeters, however collisional growth involving small particles colliding with a large target is possible, although slow (Wurm et al., 2005; Johansen et al., 2008; Windmark et al., 2012).”
Planetesimal formation by sweep-up: how the bouncing barrier can be beneficial to growth (2012, methodology): “…this fit marked by the contours in Fig.4 to the mass transfer experiments ofK the et al. (2010) (with 1 mm projectiles at velocities of 1-6 m s−1) and Wurm et al.(2005) (with 1-10 mm projectiles up to 25 m s−1) results in a rough agreement, even though our model ends up slightly pessimistic…”