Expected shape distribution of asteroids obtained from laboratory impact experiments

Fujiwara, Akira; Kamimoto, Goro; Tsukamoto, Akimasa

doi:10.1038/272602a0

Cited by 84 publications

(32 citation statements)

References 9 publications

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“…This result indicates a general property of collisional fragments which is repeated with great regularity in widely different experimental conditions such as projectile velocity, target shape, composition and strength (Fujiwara et al, 1978;Matsui et al, 1982Matsui et al, , 1984Bianchi et al, 1984;Capaccioni et al, 1984Capaccioni et al, , 1986. In general, the shape distributions of small asteroids less than tens of kilometers in diameter are considered to be similar to distributions obtained for fragments generated in laboratory impact experiments (Fujiwara et al, 1978;Capaccioni et al, 1984Capaccioni et al, , 1986.…”

Section: Introductionsupporting

confidence: 61%

The shape distribution of boulders on Asteroid 25143 Itokawa: Comparison with fragments from impact experiments

Michikami

Nakamura

Hirata

2010

Icarus

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Section: Introductionsupporting

confidence: 61%

The shape distribution of boulders on Asteroid 25143 Itokawa: Comparison with fragments from impact experiments

Michikami

Nakamura

Hirata

2010

Icarus

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“…) ratio also indicated that the fraction of fragments whose ( a b ) ratio is larger than 1.71 is about 15% (Fujiwara et al, 1978). This result implies that Nereus may be not a single fragment from a catastrophic impact in the main-belt.…”

Section: Comparison In Shape With Impact Fragmentsmentioning

confidence: 53%

“…The triaxial ratios of impact fragments produced by catastrophic disruption were investigated by laboratory impact experiments performed by Fujiwara et al, (1978) and Capaccioni et al, (1984). Both found that the average ratio of a : b : c is approximated by the simple ratio of 2 : √ 2 : 1.…”

Section: Comparison In Shape With Impact Fragmentsmentioning

confidence: 99%

Lightcurve of asteroid Nereus

2014

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An Apollo asteroid (4660) Nereus is one of the most accessible asteroids by spacecraft. Photometric observations of light variation of Nereus were performed in order to support a mission scenario planning and to elucidate the origin of the asteroid. The results revealed that Nereus has a long rotational period, 15.1 ± 1.2 hours, and that the amplitude of light variation is fairly large. Its slow rotation is preferable for a landing or touch down scenario of spacecraft. On the other hand, the comparison of lightcurve data between small main-belt asteroids and comet nuclei suggests that Nereus may be an extinct cometary nucleus, rather than a migrated asteroid from the main-belt. The comparison of the observed data with laboratory impact experiments also implies that the asteroid may not be a fragment from a catastrophic impact event in the main-belt. All the other data already obtained, such as by colorimetry, are not inconsistent with the cometary origin, either.

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“…0.2 mm sion in the near-infrared from the spectral energy distribution of HD 145263 (Sylvester & Mannings 2000) indicates that there is little hot dust, and it is difficult to expect the peak shift owing to the grain temperature effect. Very elongated forsterite ellipsoids (prolates of aspect ratio of 10-100) have the feature around 11.4 mm (Fabian et al 2001), but the presence of such grain shape is unlikely according to the experimental study of fragments from collisional disruption (Fujiwara et al 1978(Fujiwara et al , 1989Capaccioni et al 1984). Large (a few microns) crystalline forsterite grains can possibly account for the 11.44 mm shoulder.…”

Section: Observations and Data Reductionmentioning

confidence: 99%

Crystalline Silicate Feature of the Vega-like Star HD 145263

Honda

Kataza

Okamoto

et al. 2004

ApJ

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We have observed the 8-13 mm spectrum ( ) of the Vega-like star candidate HD 145263 using Subaru/ R ∼ 250 COMICS. The spectrum of HD 145263 shows the broad trapezoidal silicate feature with the shoulders at 9.3 and 11.44 mm, indicating the presence of crystalline silicate grains. This detection implies that crystalline silicate may also be commonly present around Vega-like stars. The 11.44 mm feature is slightly shifted to a longer wavelength compared to the usual 11.2-3 mm crystalline forsterite feature detected toward Herbig Ae/Be stars and T Tauri stars. Although the peak shift due to the effects of the grain size cannot be ruled out, we suggest that Fe-bearing crystalline olivine explains the observed peak wavelength fairly well. Fe-bearing silicates are commonly found in meteorites and most interplanetary dust particles, which originate from planetesimal-like asteroids. According to studies of meteorites, Fe-bearing silicate must have been formed in asteroidal planetesimals, supporting the scenario that dust grains around Vega-like stars are of planetesimal origin, if the observed 11.44 mm peak is due to Fe-bearing silicates.

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Expected shape distribution of asteroids obtained from laboratory impact experiments

Cited by 84 publications

References 9 publications

The shape distribution of boulders on Asteroid 25143 Itokawa: Comparison with fragments from impact experiments

The shape distribution of boulders on Asteroid 25143 Itokawa: Comparison with fragments from impact experiments

Lightcurve of asteroid Nereus

Crystalline Silicate Feature of the Vega-like Star HD 145263

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