Colliding Decimeter Dust

Deckers, Johannes; Teiser, Jens

doi:10.1088/0004-637x/769/2/151

Cited by 39 publications

(25 citation statements)

References 49 publications

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“…Experiments have also shown that collisions at high speeds lead to the fragmentation of the colliding dust aggregates (Blum and Münch 1993;Beitz et al 2011;Schräpler et al 2012;Deckers and Teiser 2013;. Recently, Bukhari analysed the influence of the aggregate size, size ratio and impact velocity on the outcome of fragmenting collisions.…”

Section: -Fragmentationmentioning

confidence: 99%

Dust Evolution in Protoplanetary Discs and the Formation of Planetesimals

Blum

2018

Space Sci Rev

128

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After 25 years of laboratory research on protoplanetary dust agglomeration, a consistent picture of the various processes that involve colliding dust aggregates has emerged. Besides sticking, bouncing and fragmentation, other effects, like, e.g., erosion or mass transfer, have now been extensively studied. Coagulation simulations consistently show that µm-sized dust grains can grow to mm-to cm-sized aggregates before they encounter the bouncing barrier, whereas sub-µm-sized water-ice particles can directly grow to planetesimal sizes. For siliceous materials, other processes have to be responsible for turning the dust aggregates into planetesimals. In this article, these processes are discussed, the physical properties of the emerging dusty or icy planetesimals are presented and compared to empirical evidence from within and without the Solar System. In conclusion, the formation of planetesimals by a gravitational collapse of dust "pebbles" seems the most likely.

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Section: -Fragmentationmentioning

confidence: 99%

Dust Evolution in Protoplanetary Discs and the Formation of Planetesimals

Blum

2018

Space Sci Rev

128

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“…In any case, collisions in the dense cluster of particles will also occur in these models. At the typical collision velocities of tens of m/s these collisions will definitly be destructive and lead to fragmentation into smaller particles again (Schräpler et al 2012;Deckers & Teiser 2013). The scavenging of fragments by other bodies is eventually of importance in this model as well.…”

Section: Introductionmentioning

confidence: 95%

Preplanetary scavengers: Growing tall in dust collisions

Meisner

Wurm

Teiser

et al. 2013

A&A

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Dust collisions in protoplanetary disks are one means to grow planetesimals, but the destructive or constructive nature of high speed collisions is still unsettled. In laboratory experiments, we study the self-consistent evolution of a target upon continuous impacts of submm dust aggregates at collision velocities of up to 71 m/s. Earlier studies analyzed individual collisions, which were more speculative for high velocities and low projectile masses. Here, we confirm earlier findings that high speed collisions result in mass gain of the target. We also quantify the accretion efficiency for the used SiO 2 (quartz) dust sample. For two different average masses of dust aggregates (0.29 µg and 2.67 µg) accretion efficiencies are decreasing with velocity from 58% to 18% and from 25% to 7% at 27 m/s to 71 m/s, respectively. The accretion efficiency decreases approximately as logarithmic with impact energy. At the impact velocity of 49 m/s the target acquires a volume filling factor of 38%. These data extend earlier work that pointed to the filling factor leveling off at 8 m/s to a value of 33%. Our results imply that high speed collisions are an important mode of particle evolution. It especially allows existing large bodies to grow further by scavenging smaller aggregates with high efficiency.

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“…For low velocities the coefficient of restitution decreases with increasing velocity and is constant for higher velocities before the onset of fragmentation. These studies were later continued to decimeter-sized aggregates by Deckers & Teiser (2013. In addition to studies of silica particles, the collisional behavior of water-ice particles was the subject of experimental study.…”

Section: Introductionmentioning

confidence: 99%

Influence of porosity on collisions between dust aggregates

Gunkelmann

Ringl

Urbassek

2016

A&A

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Context. Collisions between dust particles may lead to agglomerate growth or fragmentation, depending on the porosity of the dust and the collision velocity. Aims. We study the effect of agglomerate porosity and collision velocity on aggregate fragmentation and agglomeration. Methods. Granular-mechanics simulations are used to study the outcome of head-on dust aggregate collisions. The aggregates are composed of silica grains of 0.76 µm radius and have filling factors of between 0.08 and 0.21. The simulations incorporate repulsive and viscoelastic, dissipative normal forces, and intergrain adhesion. The tangential forces are composed of gliding, rolling, and torsional friction. To study the effect of aggregate porosity, we prepared spherical aggregates with identical radius but differing particle numbers. Results. The threshold velocity for agglomerate fragmentation decreases with the porosity of the aggregates. Porous aggregates tend to fragment more easily, and the fragments are irregularly shaped. In the agglomeration regime, the merged aggregate is more compact than the initial collision partners. The collision velocity at which compaction is highest is independent of the initial porosity.

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Colliding Decimeter Dust

Cited by 39 publications

References 49 publications

Dust Evolution in Protoplanetary Discs and the Formation of Planetesimals

Dust Evolution in Protoplanetary Discs and the Formation of Planetesimals

Preplanetary scavengers: Growing tall in dust collisions

Influence of porosity on collisions between dust aggregates

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