Erosion of dust aggregates

Seizinger, A.; Krijt, Sebastiaan; Kley, W.

doi:10.1051/0004-6361/201322773

Cited by 42 publications

(64 citation statements)

References 35 publications

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“…Ding et al attributed this change in rolling stiffness to the transition from pre-rolling (no contact readjustment) to true rolling motion. Figure 4 shows the observed critical rolling displacements, and compares them to predictions of (16). While the rolling displacements are orders of magnitudes larger than the atomic spacing, the results can be understood in terms of adhesion hysteresis.…”

Section: Critical Displacementmentioning

confidence: 89%

“…The inferred value of ( γ /γ ) 2.5. Unfortunately, the variation in particle radius is too small to test the correlation between ξ crit and R predicted by (16) 6 .…”

Section: Critical Displacementmentioning

confidence: 99%

“…The size of this asymmetry was assumed to equal the interatomic distance. The theory is still widely used in N -body simulations studying the behaviour of large ensembles of micrometre-sized particles [6,15,16], despite the fact that the parameter governing the asymmetry has to be increased by one to two orders of magnitude to match the experimental results.…”

Section: Introductionmentioning

confidence: 99%

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Rolling friction of adhesive microspheres

Krijt¹,

Dominik²,

Tielens³

2014

J. Phys. D: Appl. Phys.

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The rolling friction of adhesive microspheres is an important quantity as it determines the strength and stability of larger aggregates. Current models predict rolling forces that are 1 to 2 orders of magnitude smaller than observed experimentally. Starting from the well-known Johnson-Kendall-Roberts (JKR) contact description, we derive an analytical theory for the rolling friction based on the concept of adhesion hysteresis, e.g. a difference in apparent surface energies for opening/closing cracks. We show how adhesion hysteresis causes the pressure distribution within the contact to become asymmetrical, leading to an opposing torque. Analytical expressions are derived relating the size of the hysteresis, the rolling torque, and the rolling displacement, ξ . We confirm the existence of a critical rolling displacement for the onset of rolling, the size of which is set by the amount of adhesion hysteresis and the size of the contact area. We demonstrate how the developed theory is able to explain the large rolling forces and particle-size dependence observed experimentally. Good agreement with experimental results is achieved for adhesion hysteresis values of ( γ /γ ) 3 for polystyrene, and ( γ /γ ) 0.5 for silicates, at crack propagation rates of 0.1 µm s −1 and 1-10 µm s −1 , respectively.

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Section: Critical Displacementmentioning

confidence: 89%

“…The inferred value of ( γ /γ ) 2.5. Unfortunately, the variation in particle radius is too small to test the correlation between ξ crit and R predicted by (16) 6 .…”

Section: Critical Displacementmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Rolling friction of adhesive microspheres

Krijt¹,

Dominik²,

Tielens³

2014

J. Phys. D: Appl. Phys.

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“…For aggregates, N-body simulations have been performed with particles containing up to 10 6 monomers, and values of η range from close to unity (Dominik & Tielens 1997;Wada et al 2009), to several orders of magnitude less (Ringl et al 2012), and depend on the employed contact model (Seizinger et al 2013). …”

Section: Appendix A: Applicability To Aggregatesmentioning

confidence: 99%

“…For large mass ratios, s 0 acts as a projectile instead, and the largest fragment mass is set to m x /2. Collisions at mass ratios above 10 2 are assumed to be erosive (Seizinger et al 2013), with the largest fragment equalling m 0 /2. Since both the excavated mass, and the largest fragment mass, depend on the projectile, the curves in the erosive regime do not depend on the mass ratio directly.…”

Section: Appendix A: Applicability To Aggregatesmentioning

confidence: 99%

A dearth of small particles in debris disks

Krijt

Kama

2014

A&A

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Context. A prescription for the fragment size distribution resulting from dust grain collisions is essential when modelling a range of astrophysical systems, such as debris disks and planetary rings. Aims. While the slope of the fragment size distribution and the size of the largest fragment are well known, the behaviour of the distribution at the small size end is theoretically and experimentally poorly understood. This leads debris disk codes to generally assume a limit equal to, or below, the radiation blow-out size. Methods. We use energy conservation to analytically derive a lower boundary of the fragment size distribution for a range of collider mass ratios. Focusing on collisions between equal-sized bodies, we apply the method to debris disks. Results. For a given collider mass, the size of the smallest fragments is found to depend on collision velocity, material parameters, and the size of the largest fragment. We provide a physically motivated recipe for the calculation of the smallest fragment, which can be easily implemented in codes for modelling collisional systems. For plausible parameters, our results are consistent with the observed predominance of grains much larger than the blow-out size in Fomalhaut's main belt and in the Herschel cold debris disks.

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Dust Coagulation with Porosity Evolution

Kataoka

2017

Formation, Evolution, and Dynamics of Young Solar Systems

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Theoretical studies, laboratory experiments, and numerical simulations have shown several barriers in planetesimal formation, including radial drift, fragmentation, and bouncing problems. Also, observations of protoplanetary disks have shown the radial drift problems of millimeter-sized bodies at the outer orbital radius. The key to solving these problems is understanding porosity evolution. Dust grains become fluffy by coagulation in protoplanetary disks and this alters both the dynamic and optical properties of dust aggregates. First, we revealed the overall porosity evolution from micron-sized dust grains to kilometer-sized planetesimals; dust grains form extremely porous dust aggregates, where the filling factor is 10 4 , and then they are compressed by their collisions, the disk gas, and their self-gravity. In the coagulation process, they circumvent all the barriers if the monomers are 0.1-m icy bodies. The mass and porosity of the final product are consistent with those of the comets, which are believed to be the remnants of planetesimals. We further performed coagulation simulations including porosity evolution. We found that planetesimals can form inside 10 AU, avoiding the radial drift barrier. Furthermore, we calculated the opacity evolution of porous dust aggregates and found that the observed radio emission could be explained either by compact dust grains or by fluffy dust aggregates.

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Erosion of dust aggregates

Cited by 42 publications

References 35 publications

Rolling friction of adhesive microspheres

Rolling friction of adhesive microspheres

A dearth of small particles in debris disks

Dust Coagulation with Porosity Evolution

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