Size dependence of the disruption threshold: laboratory examination of millimeter–centimeter porous targets

Nakamura, Akiko; Yamane, F.; Okamoto, Takaya; Takasawa, S.

doi:10.1016/j.pss.2014.07.011

Cited by 13 publications

(10 citation statements)

References 25 publications

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“…By comparing the values of :,max / , to , , we find 0 = 0.47 ± 0.07. This value of µ B is slightly larger than that determined from laboratory impact experiments into weakly cemented basalt and highly porous gypsum, which have µ B = 0.46 [15] and 0.4 [16], respectively. Then, the value of 0 is found by setting the transition diameter between the strength and gravity regime to the size of the largest observed monolithic C-complex object: the boulder Otohime on asteroid (162173) Ryugu, which has a diameter of 160 m [17] (see Methods Eq.…”

contrasting

confidence: 56%

“…and 20 km/s (red solid line, 7 = 0.345). We compare this threshold to those of basalt (black dotted line) and pumice (black dashed line) derived from numerical simulations of impacts at angles of 45° [16,17]. b, Bennu's boulders are weaker than porous pumice (black dotted line) and non-porous basalt targets (black dashed line) of the same size.…”

Section: Figure 2 | the Maximum Crater Size On A Boulder Depends On Boulder Strengthmentioning

confidence: 99%

“…a, Using size measurements of craters on Bennu's boulders, we derived their catastrophic disruption threshold for impact speeds of 5 km/s (blue-shaded region, with variation driven by uncertainty in value of 7 ∈ [0.33,0.36]) and 20 km/s (red solid line, 7 = 0.345). We compare this threshold to those of basalt (black dotted line) and pumice (black dashed line) derived from numerical simulations of impacts at angles of 45°[16,17]. b, Bennu's boulders are weaker than porous pumice (black dotted line) and non-porous basalt targets (black dashed line) of the same size.…”

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confidence: 99%

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Bennu’s near-Earth lifetime of 1.75 million years inferred from craters on its boulders

Ballouz

Walsh

Barnouin

et al. 2020

Nature

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confidence: 56%

Section: Figure 2 | the Maximum Crater Size On A Boulder Depends On Boulder Strengthmentioning

confidence: 99%

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confidence: 99%

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Bennu’s near-Earth lifetime of 1.75 million years inferred from craters on its boulders

Ballouz

Walsh

Barnouin

et al. 2020

Nature

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“…For instance, new experimental results with a range of materials (crystalline rock, gypsum, and pyrophyllite) demonstrate that reduced porosity can increase the collisional lifetime of dust particles in interplanetary space Nakamura et al 1994Nakamura et al , 2015, especially for larger meteoroids. Figure 2 uses the results of Nakamura et al (2015) to recalculate the collisional lifetimes given in Grün et al (1985) for different materials and porosities. This is compared to the Grün et al (1985) collisional lifetimes after applying the variable F coll in Table 1.…”

Section: Collisions Modelmentioning

confidence: 99%

IMEM2: a meteoroid environment model for the inner solar system

Soja

Grün

Strub

et al. 2019

A&A

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Context. The interplanetary dust complex is currently understood to be largely the result of dust production from Jupiter-family comets, with contributions also from longer-period comets (Halley- and Oort-type) and collisionally produced asteroidal dust. Aims. Here we develop a dynamical model of the interplanetary dust cloud from these source populations in order to develop a risk and hazard assessment tool for interplanetary meteoroids in the inner solar system. Methods. The long-duration (1 Myr) integrations of dust grains from Jupiter-family and Halley-type comets and main belt asteroids were used to generate simulated distributions that were compared to COBE infrared data, meteor data, and the diameter distribution of lunar microcraters. This allowed the constraint of various model parameters. Results. We present here the first attempt at generating a model that can simultaneously describe these sets of observations. Extended collisional lifetimes are found to be necessary for larger (radius ≥ 150 μm) particles. The observations are best fit with a differential size distribution that is steep (slope = 5) for radii ≥ 150 μm, and shallower (slope = 2) for smaller particles. At the Earth the model results in ~ 90–98% Jupiter-family comet meteoroids, and small contributions from asteroidal and Halley-type comet particles. In COBE data we find an approximately 80% contribution from Jupiter-family comet meteoroids and 20% from asteroidal particles. The resulting flux at the Earth is mostly within a factor of about two to three of published measurements.

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“…Qs is obtained by impact experiments. A few sample values of G for 10 -3 kg targets at impact speed of 20 km s -1 are G = 2.2 10 5 for crystalline rock (Hörz et al, 1975) and 9 10 5 for gypsum and pyrophyllite (Nakamura et al, 2015). For porous target bodies Love et al (1993) found that G ~ (1-f) 3.6 , where f is the porosity of the target material.…”

Section: High Speed Collisionsmentioning

confidence: 99%

The Dawn of Dust Astronomy

2019

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We review the development of dust science from the first ground-based astronomical observations of dust in space to compositional analysis of individual dust particles and their source objects. A multitude of observational techniques is available for the scientific study of space dust: from meteors and interplanetary dust particles collected in the upper atmosphere to dust analyzed in situ or returned to Earth. In situ dust detectors have been developed from simple dust impact detectors determining the dust hazard in Earth orbit to dust telescopes capable of providing compositional analysis and accurate trajectory determination of individual dust particles in space. The concept of Dust Astronomy has been developed, recognizing that dust particles, like photons, carry information from remote sites in space and time. From knowledge of the dust particles' birthplace and their bulk properties, we learn about the remote environment out of which the particles were formed. Dust Observatory missions like Cassini, Stardust, and Rosetta study Saturn's satellites and rings and the dust environments of comet Wild 2 and comet Churyumov-Gerasimenko, respectively. Supplemented by simulations of dusty processes in the laboratory we are beginning to understand the dusty environments in space.

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Size dependence of the disruption threshold: laboratory examination of millimeter–centimeter porous targets

Cited by 13 publications

References 25 publications

Bennu’s near-Earth lifetime of 1.75 million years inferred from craters on its boulders

Bennu’s near-Earth lifetime of 1.75 million years inferred from craters on its boulders

IMEM2: a meteoroid environment model for the inner solar system

The Dawn of Dust Astronomy

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