Laboratory tests of catastrophic disruption of rotating bodies

Morris, A. J. W.; Burchell, M. J.

doi:10.1016/j.icarus.2017.05.016

Cited by 11 publications

(4 citation statements)

References 33 publications

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“…The distribution of particle sizes yielded by a catastrophic collision involving consolidated bodies has been studied in a number of laboratory experiments (e.g., Davis & Ryan 1990;Giacomuzzo et al 2007;Morris & Burchell 2017). The results suggest that a rollover toward small particles is common with a mass ratio of 10 −3 to 10 −4 relative to the target mass, although there is a scatter of behavior and also some level of concern that the rollover is a result of the difficulty in finding all of the smallest debris.…”

Section: Breakup Of Consolidated Bodiesmentioning

confidence: 99%

Extreme Debris Disk Variability: Exploring the Diverse Outcomes of Large Asteroid Impacts During the Era of Terrestrial Planet Formation

Jackson

Gáspár

et al. 2019

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The most dramatic phases of terrestrial planet formation are thought to be oligarchic and chaotic growth, on timescales of up to 100-200 Myr, when violent impacts occur between large planetesimals of sizes up to protoplanets. Such events are marked by the production of large amounts of debris, as has been observed in some exceptionally bright and young debris disks (termed extreme debris disks). Here we report five years of Spitzer measurements of such systems around two young solar-type stars: ID8 and P1121. The short-term (weekly to monthly) and long-term (yearly) disk variability is consistent with the aftermaths of large impacts involving large asteroid-sized bodies. We demonstrate that an impact-produced clump of optically thick dust, under the influence of the dynamical and viewing geometry effects, can produce short-term modulation in the disk light curves. The long-term disk flux variation is related to the collisional evolution within the impact-produced fragments once released into a circumstellar orbit. The time-variable behavior observed in the P1121 system is consistent with a hypervelocity impact prior to 2012 that produced vapor condensates as the dominant impact product. Two distinct short-term modulations in the ID8 system suggest two violent impacts at different times and locations. Its long-term variation is consistent with the collisional evolution of two different populations of impact-produced debris dominated by either vapor condensates or escaping boulders. The bright, variable emission from the dust produced in large impacts from extreme debris disks provides a unique opportunity to study violent events during the era of terrestrial planet formation. Subject headings: circumstellar matter -infrared: planetary systems -planets and satellites: dynamical evolution and stability -stars: individual (

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Section: Breakup Of Consolidated Bodiesmentioning

confidence: 99%

Extreme Debris Disk Variability: Exploring the Diverse Outcomes of Large Asteroid Impacts During the Era of Terrestrial Planet Formation

Jackson

Gáspár

et al. 2019

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“…The prior studies manipulated both projectile and target materials, and used basalt, glass, porous gypsum, ice, and snow to examine the effects of porosity, inclusion, and static strength on the impact strength. The size ratio of the projectile to the target, the target shape, the target rotation rate, and the impact velocity were also manipulated to elucidate how these parameters affect the impact strength and the ejection velocity of impact fragments [e.g., Gault and Wedekind, 1969;Fujiwara et al, 1977;Kawakami et al, 1983;Arakawa, 1999a;Arakawa et al, 2002;Okamoto and Arakawa, 2009;Yasui and Arakawa, 2011;Morris and Burchell, 2017]. Impact strength is defined as a specific energy when the largest fragment mass is one-half of the original target mass, and the specific energy is defined as the kinetic energy of the impactor per unit mass of the target.…”

Section: Introductionmentioning

confidence: 99%

Effects of oblique impacts on the impact strength of porous gypsum and glass spheres: Implications for the collisional disruption of planetesimals in thermal evolution

Yasui

Arakawa

Yoshida

et al. 2020

Icarus

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“…Right column: The monomers are colored according to the largest magnitude of the normal force F N exerted from its connected neighbours where F N > 0 (green) represents pushing forces while F N < 0 (red) are pulling forces, respectively. ing monomers may potentially destroy the entire aggregate in a catastrophic disruption event (Benz & Asphaug 1999;Morris & Burchell 2017;Schwartz et al 2018). What we find with our N-body simulations is that accelerated rotation deforms initially more roundish aggregates preferentially into oblate shapes.…”

Section: Rotational Deformation Of Grain Shapesmentioning

confidence: 99%

The rotational disruption of porous dust aggregates from ab-initio kinematic calculations

Reißl¹,

Nguyen²,

M.³

et al. 2023

Preprint

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Context. The sizes of dust grains in the interstellar medium follows a distribution where most of the dust mass is in smaller grains. However, the re-distribution from larger grains towards smaller sizes especially by means of rotational disruption is poorly understood. Aims. We aim to study the dynamics of porous grain aggregates under accelerated ration. Especially, we determine the deformation of the grains and the maximal angular velocity up to the rotational disruption event by caused by centrifugal forces. Methods. We pre-calculate porous grain aggregate my means of ballistic aggregation analogous to the interstellar dust as input for subsequent numerical simulations. In detail, we perform three-dimensional N-body simulations mimicking the radiative torque spinup process up to the point where the grain aggregates become rotationally disrupted. Results. Our simulations results are in agreement with theoretical models predicting a characteristic angular velocity ω disr of the order of 10 8 − 10 9 rad s −1 , where grains become rotationally disrupted. In contrast to the theoretical predictions, we show that for large porous grain aggregates ( 300 nm) ω disr does not strictly decline but reaches a lower asymptotic value. Hence, such grains can withstand an accelerated ration more efficiently up to a factor of 10 because the displacement of mass by centrifugal forces and the subsequent mechanical deformation supports the build up of new connections within the aggregate. Furthermore, we report that the rapid rotation of grains deforms an ensemble with initially 50:50 prolate and oblate shapes, respectively, preferentially into oblate shapes. Finally, we present a best fit formula to predict the average rotational disruption of an ensemble of porous dust aggregates dependent on internal grain structure, total number of monomers, and applied material properties.

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Laboratory tests of catastrophic disruption of rotating bodies

Cited by 11 publications

References 33 publications

Extreme Debris Disk Variability: Exploring the Diverse Outcomes of Large Asteroid Impacts During the Era of Terrestrial Planet Formation

Extreme Debris Disk Variability: Exploring the Diverse Outcomes of Large Asteroid Impacts During the Era of Terrestrial Planet Formation

Effects of oblique impacts on the impact strength of porous gypsum and glass spheres: Implications for the collisional disruption of planetesimals in thermal evolution

The rotational disruption of porous dust aggregates from ab-initio kinematic calculations

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