Collisional Processes of Iron and Steel Projectiles on Targets of Different Densities

Fechtig, H.; Nagel, K.; Pailer, N.; Schneider, E.

doi:10.1007/978-94-009-9102-6_71

Cited by 8 publications

(4 citation statements)

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“…Assuming a low density for loess of ρ t = 1600 kg m −3 and using σ p = 150 and 800 MPa as the upper limit strength of the largest funnel‐forming fragments of 30 t, following the Weibull law for α values of 0.25 and 0.1, the critical impact velocity V fin is ~300 and ~700 m s −1 . Using experimental data (Fechtig et al., 1980; Kadono, 1999), and interpolating to the same projectile target density ratio, a higher value of V fin ~ 1 km s −1 could be derived. This is probably the upper limit of impact velocity which allows high‐strength iron meteoroids impacting loess to survive.…”

Section: Resultsmentioning

confidence: 99%

Campo del Cielo modeling and comparison with observations: I. Atmospheric entry of the iron meteoroid

Schmalen

Luther

Artemieva

2022

Meteorit & Planetary Scien

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This paper presents an attempt to reconstruct the Campo del Cielo (CdC) impact event, that is, to estimate the preatmospheric mass and velocity of the iron meteoroid and pre-impact parameters of its fragments allowing formation of funnels and impact craters. The goal of this study is to improve the understanding of the effects small-scale iron meteoroids can have on the Earth's surface. We model the meteoroid's atmospheric flight taking deceleration, ablation, and fragmentation into account, and then compare the results with available observations. We found that a fragment's velocity near the surface should be <1 km s −1 in order to form a funnel with an intact meteorite inside. The estimates of preatmospheric (at an altitude of 100 km) parameters of the CdC impact event are as follows: minimal mass of 7500-8500 t, which corresponds to a diameter range of 12.2-12.8 m; maximum entry angle above the atmosphere of ~16.5°and velocities of 14.5-18.4 km s −1 , which is close to the one most frequently reached by Near-Earth objects (NEOs). Near the surface, the largest fragments with a mass of 400-1500 t and velocities of 4-7 km s −1 form impact craters whereas fragments with a mass <31 t and velocities <1 km s −1 form funnels. Masses <3 t are not included in our simulations. Their total mass is 280-460 t at the point of disruption but <110 t on the Earth's surface. These numerous small fragments are dispersed over a large area and are very popular among meteorite hunters and dealers. In spite of all the observed crater location/size data and impactor velocity limits from the models, there are far more free parameters than constraints. As a result, any values for preatmospheric mass, velocity, and entry angle are merely representative or limitative as opposed to true values.

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Section: Resultsmentioning

confidence: 99%

Campo del Cielo modeling and comparison with observations: I. Atmospheric entry of the iron meteoroid

Schmalen

Luther

Artemieva

2022

Meteorit & Planetary Scien

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“…The track lengths, L t , for the three Stardust tracks were calculated from this model (Table 1) with an assumed average aerogel density (5 mg/ cm 3 ) and the estimated projectile sizes, d p , and density, ρ p (L t,calc in Table 1). They are sufficiently larger than the real Ishibashi et al (1990) (nylon projectiles into foamed polystyrene targets), Fechtig et al (1980) and Werle et al (1981) (steel projectiles into porous alumina target), Cannon and Turner (1967) (nylon, magnesium, aluminum and steel projectiles into polyurethane foam targets), Barrett et al (1992) (olivine projectiles into aerogel targets), Tsou (1990) (aluminum projectiles into polystyrene, polyimide, polyethylene, and polyacrylonitrile form targets), and Love et al (1993) (soda lime glass projectiles into sintered soda lime glass beads target) were compiled by Kadono et al (1999). Experiments of Burchell et al (2008) used soda lime glass projectiles into Stardust-grade aerogel targets at 5.8-6.1 km/s.…”

Section: Estimation Of Impact Particle Mass and Sizementioning

confidence: 98%

Three‐dimensional structures and elemental distributions of Stardust impact tracks using synchrotron microtomography and X‐ray fluorescence analysis

Tsuchiyama¹,

Nakamura²,

Okazaki³

et al. 2009

Meteorit & Planetary Scien

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available online at http://meteoritics.org Abstract-Three-dimensional structures and elemental abundances of four impact tracks in silica aerogel keystones of Stardust samples from comet 81P/Wild 2 (bulbous track 67 and carrot-type tracks 46, 47, and 68) were examined non-destructively by synchrotron radiation-based microtomography and X-ray fluorescence analysis. Track features, such as lengths, volumes and width as a function of track depth, were obtained quantitatively by tomography. A bulbous portion was present near the track entrance even in carrot-type tracks. Each impact of a cometary dust particle results in the particle disaggregated into small pieces that were widely distributed on the track walls as well as at its terminal. Fe, S, Ca, Ni, and eight minor elements are concentrated in the bulbous portion of track 68 as well as in terminal grains. It was confirmed that bulbous portions and thin tracks were formed by disaggregation of very fine fragile materials and relatively coarse crystalline particles, respectively. The almost constant ratio of whole Fe mass to track volume indicates that the track volume is almost proportional to the impact kinetic energy. The size of the original impactor was estimated from the absolute Fe mass by assuming its Fe content (CI) and bulk density. Relations between the track sizes normalized by the impactor size and impact conditions are roughly consistent with those of previous hypervelocity impact experiments. Three-dimensional structures and elemental distributions of Stardust impact tracks using synchrotron microtomography and X-ray fluorescence analysis

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“…For more quantitative description, the depth L and the maximum diameter D m of final tracks are often measured as a function of the parameters varied in the experiments such as, projectile density q p , projectile diameter D p (radius R p ), projectile and target strengths, target density q t , and impact velocity v 0 . The features about L/D p and D m suggested by previous various experiments with low-density targets are roughly summarized as follows: L/D p increases with v 0 , and takes a peak, then decreases (e.g., Fechtig et al, 1980;Werle et al, 1981;Ishibashi et al, 1990;Tsou, 1990; Barrett et al, 1992;Kitazawa et al, 1999;Burchell et al, 2001;Hörz et al, 2009), and is scaled by q p /q t (e.g., Barrett et al, 1992;Hörz et al, 1993;Love et al, 1993;Burchell et al, 1999Burchell et al, , 2009Niimi et al, 2011Niimi et al, , 2012, and D m is proportional to D p regardless of q p /q t and proportional to v 0 (e.g., Ishibashi et al, 1990;Kitazawa et al, 1999;Burchell et al, 2008;Niimi et al, 2012).…”

Section: Introductionmentioning

confidence: 96%

“…Hypervelocity impact experiments on very low-density materials have been carried out to extend the cratering experiments (e.g., Cannon and Turner, 1967;Fechtig et al, 1980;Werle et al, 1981;Love et al, 1993;Trucano and Grady, 1995) and to develop and calibrate the instruments for intact capture of interplanetary dust samples using foams (e.g., Ishibashi et al, 1990;Tsou, 1990) and for aerogels (e.g., Barrett et al, 1992;Hörz et al, 1993Hörz et al, , 1998Hörz et al, , 2009Burchell et al, 1999Burchell et al, , 2001Burchell et al, , 2008Burchell et al, , 2009Kitazawa et al, 1999;Niimi et al, 2011Niimi et al, , 2012. These previous studies indicate that the impacts between high-density projectiles and low-density targets generate ''penetration tracks'': track diameter is small at the entrance (= impact point), then increases with depth, takes a peak, and decreases (this qualitative feature is common for any track).…”

Section: Introductionmentioning

confidence: 99%

Penetration into low-density media: In situ observation of penetration process of various projectiles

Kadono

Niimi

Okudaira

et al. 2012

Icarus

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Collisional Processes of Iron and Steel Projectiles on Targets of Different Densities

Cited by 8 publications

References 4 publications

Campo del Cielo modeling and comparison with observations: I. Atmospheric entry of the iron meteoroid

Campo del Cielo modeling and comparison with observations: I. Atmospheric entry of the iron meteoroid

Three‐dimensional structures and elemental distributions of Stardust impact tracks using synchrotron microtomography and X‐ray fluorescence analysis

Penetration into low-density media: In situ observation of penetration process of various projectiles

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