The fall and recovery of the Tagish Lake meteorite

Hildebrand, A. R.; McCausland, Phil J.A.; Brown, Peter; Longstaffe, Fred J.; Russell, S.; Tagliaferri, E.; Wacker, J. F.; Mazur, Michael J.

doi:10.1111/j.1945-5100.2006.tb00471.x

Cited by 97 publications

(109 citation statements)

References 44 publications

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“…Whole-rock d 18 O and d 17 O values of the Tagish Lake meteorite range from 16.9& to 23.5&, and 8.5& to 12.2&, respectively (Brown et al, 2000;Clayton and Mayeda, 2001;Hildebrand et al, 2006). These compositions are enriched in 18 O and 17 O compared to CM chondrites and are similar to those of CI chondrites (Clayton and Mayeda, 1999).…”

Section: Introductionmentioning

confidence: 57%

The oxygen-isotope composition of chondrules and isolated forsterite and olivine grains from the Tagish Lake carbonaceous chondrite

Russell

Longstaffe

King

et al. 2010

Geochimica et Cosmochimica Acta

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Section: Introductionmentioning

confidence: 57%

The oxygen-isotope composition of chondrules and isolated forsterite and olivine grains from the Tagish Lake carbonaceous chondrite

Russell

Longstaffe

King

et al. 2010

Geochimica et Cosmochimica Acta

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“…Flynn (2004) has further considered the effect of porosity on mechanical strength, and identifies an "atmospheric filter," arguing that meteorites with high porosity are likely to preferentially undergo fragmentation during atmospheric ablation. The high-porosity Tagish Lake meteorite (Hildebrand et al 2006) with φ ~40%, for example, produced an extensive strewn field composed of many thousands of fragments, indicative of a very weak parent body. This being said, found no correlation between porosity and sample size (for a mass range varying from 0.002 to 2 kg).…”

Section: Discussionmentioning

confidence: 99%

Physical properties of Martian meteorites: Porosity and density measurements

Coulson

Beech

Nie

2007

Meteorit & Planetary Scien

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Abstract-Martian meteorites are fragments of the Martian crust. These samples represent igneous rocks, much like basalt. As such, many laboratory techniques designed for the study of Earth materials have been applied to these meteorites. Despite numerous studies of Martian meteorites, little data exists on their basic structural characteristics, such as porosity or density, information that is important in interpreting their origin, shock modification, and cosmic ray exposure history. Analysis of these meteorites provides both insight into the various lithologies present as well as the impact history of the planet's surface. We present new data relating to the physical characteristics of twelve Martian meteorites. Porosity was determined via a combination of scanning electron microscope (SEM) imagery/image analysis and helium pycnometry, coupled with a modified Archimedean method for bulk density measurements. Our results show a range in porosity and density values and that porosity tends to increase toward the edge of the sample. Preliminary interpretation of the data demonstrates good agreement between porosity measured at 100× and 300× magnification for the shergottite group, while others exhibit more variability. In comparison with the limited existing data for Martian meteorites we find fairly good agreement, although our porosity values typically lie at the low end of published values. Surprisingly, despite the increased data set, there is little by way of correlation between either porosity or density with parameters such as shock effect or terrestrial residency. Further data collection on additional meteorite samples is required before more definitive statements can be made concerning the validity of these observations.

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“…These meteorite properties are probably representative for the original Tagish Lake meteoroid (Hildebrand et al 2006). The Almahata Sitta meteorites produced by 2008 TC 3 are rare ureilites with varying bulk densities of 2100-2500 kg m −3 and porosities 25-37% (Jenniskens et al 2009).…”

Section: Discussionmentioning

confidence: 99%

Meteosat observation of the atmospheric entry of 2008 TC$\mathsf{_{3}}$ over Sudan and the associated dust cloud

Borovička¹,

Charvát²

2009

A&A

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We analyzed serendipitous observations by the Meteosat 8 weather satellite of the fireball caused by the entry of the small asteroid (or large meteoroid) 2008 TC 3 over northern Sudan on October 7, 2008. Meteosat 8 scans the Earth in 5 min cycles. The fireball was captured in the 2:45 UT images in four visible-near infrared channels (0.6-1.6 μm) at a height of 45 km, and in eight mid infrared channels (3.9-13.4 μm) at a height of 33 km. The latter channels also detected at least two dust clouds deposited in the atmosphere at the heights of about 44 and 36 km. The dust deposition was a result of severe atmospheric fragmentation of the asteroid, accompanied by fireball flares, which could be detected in the light scattered by the Earth's surface. The fireball brightness was measured at two random heights, 45 and 37.5 km, where it reached −18.8 and −19.7 mag, respectively. The peak brightness was probably higher than −20 mag. The color temperature of the fireball at 45 km was 3650 ± 100 K. Infrared spectra of the fresh dust clouds were dominated by the 10 μm Si-O band caused by recondensed amorphous silicates. Five minutes later, the dust clouds were detected in absorption of thermal radiation of the Earth. At that time, the silicates were largely crystalline, suggesting silicate smoke temperatures exceeding 1000 K. The total mass of the silicate smoke was estimated to be 3100 ± 600 kg. More mass was probably contained in larger, micron sized, and colder dust particles resulting from incomplete sublimation of the asteroidal material and detected later by Meteosat 8 and 9 in scattered sunlight. Based on the heights of asteroid fragmentations, we guess that the bulk porosity of 2008 TC 3 was of the order of 50%, i.e. higher than the porosity of the recovered meteorite Almahata Sitta.

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The fall and recovery of the Tagish Lake meteorite

Cited by 97 publications

References 44 publications

The oxygen-isotope composition of chondrules and isolated forsterite and olivine grains from the Tagish Lake carbonaceous chondrite

The oxygen-isotope composition of chondrules and isolated forsterite and olivine grains from the Tagish Lake carbonaceous chondrite

Physical properties of Martian meteorites: Porosity and density measurements

Meteosat observation of the atmospheric entry of 2008 TC$\mathsf{_{3}}$ over Sudan and the associated dust cloud

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