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Brown, P T; Campbell, Margaret D.; Ellis, K.J.; Hawkes, R. L.; Jones, J.; Gural, Peter S.; Babcock, D.; Barnbaum, C.; Bartlett, R. K.; Bedard, M.; Bedient, J.; Beech, Martin; Brosch, Noah; Clifton, S.; Connors, Martin; Cooke, Bill; Goetz, P.; Gaines, J. K.; Gramer, Lewis J.; Gray, John E.; Hildebrand, A. R.; Jewell, D.; Jones, A. R.; Leake, M. A.; LeBlanc, Andrew Glenn; Looper, J. K.; McIntosh, B.A.; Montague, T.; Morrow, M. J.; Murray, Ian S.; Nikolova, Simona; Robichaud, Janine; Spondor, R.; Talarico, J.; Theijsmeijer, C.; Tilton, B.; Treu, M.; Vachon, C.; Webster, A. R.; Weryk, R.; Worden, Simon P.

doi:10.1023/a:1017024802184

Cited by 6 publications

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“…Sarma & Jones (1985) found k = 5 and k = 9 km, respectively, using two different camera systems on sporadic meteors of the similar mass range. Brown et al (2000) found k = 9 km for single station 1999 Leonids.…”

Section: Classification and Ablation Of Small Meteoroidsmentioning

confidence: 96%

Physical and chemical properties of meteoroids as deduced from observations

Borovička

2005

Proc. IAU

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A review of the current knowledge of physical properties and chemical composition of meteoroids entering the Earth's atmosphere is presented. Meteoroid penetration ability, ablation coefficients, beginning heights, light curves, fragmentation, and spectra are considered. The inferred bulk densities, mechanical strengths, rotation, and atomic elemental abundances are discussed. Cometary meteoroids are effectively grain aggregates with low bulk density (100-1000 kg m −3), high porosity and low cohesivity. A volatile matrix holding the grains together may be present. Presence of large amounts of organic material is not firmly established. Small chunks (∼1 mm) of denser material are sometimes contained in cometary meteoroids. Chemically, cometary grains are similar to CI chondrites but there is a hint of enhancement of Na, Si, and Mg and depletion of Fe, Cr, and Mg. Larger chemical diversity is observed among small meteoroids on cometary orbits not belonging to meteoroid streams. The relatively frequent Na-free meteoroids are probably fragments of cometary irradiation crust. Asteroidal meteoroids exhibit much lower mechanical strengths than stony meteorites, clearly due to the presence of large scale cracks. Iron meteoroids dominate among asteroidal meteoroids smaller than 1 cm.

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Section: Classification and Ablation Of Small Meteoroidsmentioning

confidence: 96%

Physical and chemical properties of meteoroids as deduced from observations

Borovička

2005

Proc. IAU

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Discoveries from Observations and Modeling of the 1998/99 Leonids

Jenniskens

2001

Astronomy and Astrophysics Library

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The 1999 Leonid Multi-Instrument Aircraft Campaign — An Early Review

Jenniskens

Butow

Fonda

2000

Leonid Storm Research

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The Leonid meteor storm of 1999 was observed from two B707-type research aircraft by a team of 35 scientists of seven nationalities over the Mediterranean Sea on Nov. 18, 1999. The mission was sponsored by various science programs of NASA, and offered the best possible observing conditions, free of clouds and at a prime location for viewing the storm. The 1999 mission followed a similar effort in 1998, improving upon mission strategy and scope. As before, spectroscopic and imaging experiments targeted meteors and persistent trains, but also airglow, aurora, elves and sprites. The research aimed to address outstanding questions in Planetary Science, Astronomy, Astrobiology and upper atmospheric research, including Aeronomie. In addition, near real-time flux measurements contributed to a USAF sponsored program for space weather awareness. An overview of the first results is given, which are discussed in preparation for future missions.

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Cited by 6 publications

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Physical and chemical properties of meteoroids as deduced from observations

Physical and chemical properties of meteoroids as deduced from observations

Discoveries from Observations and Modeling of the 1998/99 Leonids

The 1999 Leonid Multi-Instrument Aircraft Campaign — An Early Review

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