Shedding of dust rims in chondrule collisions in the protoplanetary disk

Umstätter, Philipp; Gunkelmann, Nina; Dullemond, C. P.; Urbassek, Herbert M.

doi:10.1093/mnras/sty3431

Cited by 5 publications

(12 citation statements)

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“…if the surface is semi-molten due to external heating then microchondrules may also be produced by this process. We note that collisions with other chondrules may also be part of the erosive process (e.g., Umstätter et al (2019)), but we do not consider interchondrule collisions in this paper.…”

Section: Kinetic Fgr Formationmentioning

confidence: 99%

Fine-grained rim formation – High speed, kinetic dust aggregation in the early Solar System

Liffman

2019

Geochimica et Cosmochimica Acta

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Type 3 chondritic meteorites often contain chondrules and refractory inclusions that are coated with accretionary, fine-grained rims (FGRs). FGRs are of low porosity, were subject to centrally directed pressure, may contain high temperature products like microchondrules and there is a linear relationship between the rim thickness and the radius of the enclosed object.FGRs are thought to have formed by the gentle adhesion of dust onto the central object with the subsequent compression of this fluffy rim within the parent body. However, this model does not explain the low porosity, micro-chondrules and centralized pressure. This model also has difficulties explaining the linear relationship between rim thickness and object size including the existence of a non-zero constant in that linear relationship.We propose that FGRs formed by the relatively high-speed interaction between dust and the object, where high initial impact speed produced abrasion and, possibly, microchondrules. FGR formation occurred over a range of lower speeds aided by vacuum adhesion of fragments from the impacting dust particles. This model naturally produces the rim thickness linear relationship with non-zero constant, low porosity and centrally directed pressure. We call this process kinetic dust aggregation (KDA), which is another name for the aerosol deposition processes used in industry. KDA may be a tentative, part explanation of how dust aggregation occurs in protostellar disks on the pathway from dust to planets.

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Section: Kinetic Fgr Formationmentioning

confidence: 99%

Fine-grained rim formation – High speed, kinetic dust aggregation in the early Solar System

Liffman

2019

Geochimica et Cosmochimica Acta

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“…Some of the linear relationships observed in CM chondrites are consistent with our estimation, but the rim thicknesses around CM Murray and CM Murchison are smaller than our estimation. The chondrules in these CM chondrites would lose their surrounding dust rims in the latter accretion processes such as collisions between chondrules with rims (Umstätter et al, 2019) and collision-induced chondrule ejection (Arakawa, 2017). The thickness of the rims would be affected by the high-velocity collisions and subsequent fragments accretion (Liffman, 2019).…”

Section: Discussionmentioning

confidence: 99%

“…Rims are, however, stripped in subsequent collisions. Rim grains are lost in collisions between chondrules with rims (Umstätter et al, 2019), and high-velocity collisions induce chondrule ejection from aggregates (Arakawa, 2017). We ignore these subsequent events and give an upper limit estimation of rim thicknesses.…”

Section: Overviewmentioning

confidence: 99%

Formation of rims around chondrules via porous aggregate accretion

Matsumoto,

Hasegawa,

Matsuda

et al. 2021

Preprint

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Chondrules are often surrounded by fine-grained rims or igneous rims. The properties of these rims reflect their formation histories. While the formation of fine-grained rims is modeled by the accretion of dust grains onto chondrules, the accretion should be followed by the growth of dust grains due to the shorter growth timescale than the accretion. In this paper, we investigate the formation of rims, taking into account the growth of porous dust aggregates. We estimate the rim thickness as a function of the chondrule fraction at a time when dust aggregate accretion onto chondrules is switched to collisions between these chondrules. Our estimations are consistent with the measured thicknesses of finegrained rims in ordinary chondrites. However, those of igneous rims are thicker than our estimations. The thickness of igneous rims would be enlarged in remelting events.

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“…This work uses the same model as previous works (e.g., Ringl & Urbassek (2012), Ringl et al (2012a), Gunkelmann et al (2016), Umstätter et al (2019)). We review this model here for convenience and completeness.…”

Section: Granular Mechanicsmentioning

confidence: 99%

Fragmentation and energy dissipation in collisions of polydisperse granular clusters

Umstätter

Urbassek

2020

A&A

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Context. Dust aggregates consist of polydisperse grains following a power-law size distribution with an exponent of around 2.5, called the Mathis-Rumpl-Nordsieck (MRN) distribution. Aims. We compare the outcome of collisions between polydisperse granular aggregates with those of monodisperse aggregates. Methods. Granular-mechanics simulations were used to study aggregate collisions. Results. Both with respect to the fragmentation threshold and to energy dissipation, MRN aggregates behave as monodisperse aggregates if their size corresponds approximately to the geometric mean of the largest and smallest radius of the MRN distribution. Conclusions. Our results allow the polydisperse aggregates to be substituted with monodisperse aggregates, which are easier to simulate.

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Shedding of dust rims in chondrule collisions in the protoplanetary disk

Cited by 5 publications

References 0 publications

Fine-grained rim formation – High speed, kinetic dust aggregation in the early Solar System

Fine-grained rim formation – High speed, kinetic dust aggregation in the early Solar System

Formation of rims around chondrules via porous aggregate accretion

Fragmentation and energy dissipation in collisions of polydisperse granular clusters

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