Impact fragmentation experiments of basalts and pyrophyllites

Takagi, Y.; Mizutani, Hitoshi; Kawakami, Shin‐ichi

doi:10.1016/0019-1035(84)90114-3

Cited by 105 publications

(105 citation statements)

References 10 publications

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“…The dotted line shows the relation for 0% porosity. Basalt data were based on previous studies; 1 : Fujiwara et al (1977) with impact velocity of 2500-2900 m/s, 2: Matsui et al (1982) with 50-150 m/s, 3: Takagi et al (1984) with 70-990 m/s. The initial peak pressure, P 0 , of each experiment is shown in parenthesis.…”

Section: Resultsmentioning

confidence: 99%

“…As suggested by previous studies (Takagi et al, 1984;Ryan et al, 1999), the conclusions drawn from high-velocity impact experiments cannot simply be applied to impacts at low velocities. For example, the peak pressure at an impact does not scale in a straightforward fashion with Q, because the dependence of the peak pressure at impact velocity is approximately linear under low-velocity conditions but quadratic at extremely high velocities.…”

Section: Introductionmentioning

confidence: 90%

“…For example, the peak pressure at an impact does not scale in a straightforward fashion with Q, because the dependence of the peak pressure at impact velocity is approximately linear under low-velocity conditions but quadratic at extremely high velocities. Takagi et al (1984) introduced another scaling parameter, P I , instead of Q, for characterizing collisional experiments of different projectile and target materials and impact velocities. The scaling parameter, called the non-dimensional impact stress (NDIS) is given in the form of…”

Section: Introductionmentioning

confidence: 99%

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Collisional disruption of weakly sintered porous targets at low-impact velocities

et al. 2007

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Porous structure is common in the asteroids and satellites of the outer planets. In order to study the relationship between the structure of small bodies and their thermal and collisional evolution, we performed impact disruption experiments on porous sintered targets using a light-gas gun at velocities ranging from 10 to 100 m/s. The sintered glass bead targets were prepared to have roughly the same porosity but with different compressive strengths, ranging over an order of magnitude, by controlling sintering duration and temperature. The results of the impact experiments show that the targets of higher compressive strength have higher impact strengths. However, compared to previous results on impact disruption of porous sintered targets with a collisional velocity of approximately 6 km/s, the values of impact strength in this study were found to be lower by an order of magnitude.

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Section: Resultsmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 90%

Section: Introductionmentioning

confidence: 99%

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Collisional disruption of weakly sintered porous targets at low-impact velocities

et al. 2007

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“…Depending on the ratio of the impact energy to the critical energy, the average size of the fragments changes. This has been measured (e.g., Takagi et al 1984) and numerically modeled (e.g., Durda et al 2007), and useful analytic prescriptions for use in collisional codes are available (e.g., Thébault & Augereau 2007). Here we apply a simplified approach with only one parameter, the slope η of a single power law dN ∝ m −η dm.…”

Section: Dynamical and Collisional Evolutionmentioning

confidence: 99%

The Debris Disk of Vega: A Steady-State Collisional Cascade, Naturally

Müller

Löhne

Krivov

2009

ApJ

102

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The archetypical debris disk around Vega has been observed intensively over the past 25 years. It has been argued that the resulting photometric data and images may be in contradiction with a standard, steady-state collisional scenario of the disk evolution. In particular, the emission in the mid-infrared (mid-IR) appears to be in excess of what is expected from a "Kuiper belt" at ∼100 AU, which is evident in the submillimeter images and inferred from the majority of photometric points. Here we re-address the question of whether or not the Vega disk observations are compatible with a continuous dust production through a collisional cascade. Instead of seeking a size and spatial distribution of dust that provide the best fit to observations, our approach involves physical modeling of the debris disk "from the sources." We assume that dust is maintained by a belt of parent planetesimals, and employ our collisional and radiative transfer codes to consistently model the size and radial distribution of the disk material and then thermal emission of dust. In doing so, we vary a broad set of parameters, including the stellar properties, the exact location, extension, and dynamical excitation of the planetesimal belt, chemical composition of solids, and the collisional prescription. We are able to reproduce the spectral energy distribution in the entire wavelength range from the near-IR to millimeter, as well as the mid-IR and submillimeter radial brightness profiles of the Vega disk. Thus, our results suggest that the Vega disk observations are not in contradiction with a steady-state collisional dust production, and we put important constraints on the disk parameters and physical processes that sustain it. The total disk mass in 100 km-sized bodies is estimated to be ∼10 Earth masses. Provided that collisional cascade has been operating over much of the Vega age of ∼350 Myr, the disk must have lost a few Earth masses of solids during that time. We also demonstrate that using an intermediate luminosity of the star between the pole and the equator, as derived from its fast rotation, is required to reproduce the debris disk observations. Finally, we show that including cratering collisions into the model is mandatory.

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“…The smaller end of the size distribution has received considerably less attention; the smallest fragments are hard to count experimentally, and require a very high resolution to be captured in numerical simulations. Fragment distributions are therefore incomplete below sizes of 100 µm, or masses below 10 −3 gr (Fujiwara et al 1977;Takagi et al 1984). Molecular dynamics (e.g.…”

Section: Introductionmentioning

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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Impact fragmentation experiments of basalts and pyrophyllites

Cited by 105 publications

References 10 publications

Collisional disruption of weakly sintered porous targets at low-impact velocities

Collisional disruption of weakly sintered porous targets at low-impact velocities

The Debris Disk of Vega: A Steady-State Collisional Cascade, Naturally

A dearth of small particles in debris disks

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