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A small oriented Chelyabinsk meteorite, weighing 0.3 grams.

This Chelyabinsk meteorite is a flight-oriented individual; a small, fusion-crusted 'button' with roll-over lipping on the trailing side.
For scale, the cube in the lower right image has sides of 1 cm (10 mm). The ticks on the ruler in the other two pictures are 1 mm apart. The tiny 'button' meteorite is only 8 mm by 9 mm across.

After the large meteoroid broke-up explosively during its passage through the Earth's atmosphere, thousands of small fragments fell to earth. Most fragments tumbled randomly, but a very few had a shape that allowed them to maintain a stable orientation as they fell. This small stone would have maintained a stable flight-orientation with the leading or forward side developing a convex (curved outwards) shape as material melted and ablated away. Some of this ablated material rolled over in the high-speed airflow onto the flatter, trailing side creating the 'roll-over lip' around its rim. Also, the fusion crust on the trailing side is rather frothy due to lower pressure on the object's trailing side.

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Chelyabinsk

Observed fall: 15 February 2013, 9.22 a.m. (03.22 UTC), Chelyabinskya oblast, Russia.

Approximate centre of the strewn-field: 54° 49' N; 61° 07' E.

Total Known Mass: ~ 1000 kg.

Classification: Ordinary chondrite, LL5.
Shock stage: S4.
Weathering grade: W0.

Fayalite (mol%): 27.9 +/- 0.36 (N=22).
Ferrosilite (mol%): 22.8 +/- 0.79 (N=17).
Wollastonite (mol%): 1.3 +/- 0.26 (N=17).
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At about 09.20 local time on 15 February 2013, a small asteroid / large meteoroid, travelling at 30 km/s and estimated to have been approximately 17 - 20 metres in diameter with a mass of around 10,000 tonnes, entered the Earth's atmosphere at a shallow 18-degree angle over the southern Ural region of Russia. As it slowed in the atmosphere to around 19 km/s the light from the bright fireball - or superbolide - was briefly brighter than the Sun, and was visible around sunrise over a wide area as well as being captured on many video cameras.

The object exploded in an air-burst over Chelyabinsk oblast at a height of about 30 km. The explosion generated a bright flash, producing a hot cloud of dust and gas that penetrated to 26 km, and many surviving small fragments of the meteoroid which continued to fall to earth. Residents of the Chelyabinsk district heard the loud detonation, and the shock wave of the airburst damaged many buildings in Chelyabinsk and surrounding towns. Many people were injured by glass fragments from broken windows. The asteroid / meteoroid was the largest object to have entered the Earth's atmosphere since the 1908 Tunguska event in Siberia.

Further explosions and fragmentation of large fragments occurred to an altitude of about 18 km and thousands of meteorite stones fell as a shower around Pervomaiskoe, Deputatsky and Yemanzhelinka villages, about 40 km south of Chelyabinsk. Snow (about 0.7 metre deep) covered the ground, and the meteorite pieces were collected out of the snow by local people soon after the fall. The falling stones formed holes surrounded by firm snow. The largest stones reached the frozen soil. It is estimated that the total mass collected by local people exceeds 100 kg and may be up to 500 kg.

The main mass of the Chelyabinsk meteorite fell into Chebarkul Lake. Numerous small meteorite fragments (~ 0.5 to 1 g) were found scattered around a 7-metre wide hole (54° 57' 33.74" N; 60° 19' 19.58" E) in the snowy ice covering the lake, located 70 km west of Chelyabinsk. 5 kg of meteorite samples were recovered from the lake bottom using magnets during the first month after the fall. Additionally, around 10 kg of fragments were recovered by local residents in the same way (but were not well documented). Underwater recovery operations in September and October 2013 retrieved eight meteorite fragments; the largest weighed ~ 540 kg. The other seven fragments totalled 84.4 kg. the total mass of meteorite pieces recovered from the bottom of Chebarkul Lake was therefore around 640 kg. The total mass of fragments recovered from the lake and collected on land in the strewn-field is estimated to be around 1000 kg.

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Octahedrite from the Asteroid Belt between Mars and Jupiter. (USNM 1492, National Museum of Natural History (Smithsonian Institution), Washington D.C., USA) (public domain image provided by the USNM)

Meteorites are rocks from space. Three basic categories exist: 1) stony meteorites; 2) iron meteorites; and 3) stony-iron meteorites. As the name suggests, iron meteorites are dominated by iron metal (elemental Fe). They also include some metallic nickel (Ni), plus minor minerals. They represent metallic core samples from differentiated asteroids/dwarf planets in the Solar System that have been disrupted by one or more large impact events.

Iron meteorites come in three textural varieties: octahedrites, hexahedrites, and ataxites. Octahedrites are the most common type of Fe-Ni meteorites. The textural classification of iron meteorites has been augmented with information on trace element content.

Mineralogically, all octahedrites are dominated by two minerals having very similar chemistries: kamacite (FeNi) and taenite (FeNi). Kamacite is a silvery-colored iron-nickel metal alloy rich in iron, with about 5.5 weight-percent nickel. Taenite is a silvery-colored iron-nickel metal alloy rich in nickel, with about 27-65 weight-percent nickel. Octahedrites have much more kamacite than taenite. They also contain minor amounts of troilite (FeS - iron monosulfide), silicate minerals, and others.

The physical crystalline structure of octahedrites is distinctive. On cut, polished, and nitric acid-etched surfaces, a criss-crossing pattern of silvery-gray blades is evident. This is called Widmanstätten structure, formed when kamacite and taenite slowly crystallized from cooling magma. The two minerals form interlocking plates with octahedral (double pyramid) geometries.

The octahedrite seen here is an oriented individual of the Henbury Meteorite, which was found west-southwest of the "town" of Henbury, Northern Territory, central Australia. Many samples were collected in the 1930s from a crater field consisting of 14 small to moderately small impact craters. The impact event occurred during the Holocene, at about 4.2 ka. The target rocks are Precambrian fine-grained siliciclastic sedimentary rocks. The meteorite itself is a medium octahedrite. This specimen has a fusion crust and abundant regmaglypts. Henbury is classified as a group IIIAB iron meteorite.

A striking urban scene featuring a blue door against a gray wall, complemented by an orange pole. The image highlights the textures and colors of the materials in a minimalist composition.

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Details best viewed in Original Size.

St. Anne's Church is a Roman Catholic Church located in the Śródmieście district, the main center of academic chaplaincy in Warsaw. The church was built at the Bernardine monastery, which was founded by Princess Anna Fyodorówna. In 1454, through the intermediary of John of Capistrano, she brought the first monks to Warsaw. Six brothers came to Warsaw under the leadership of Fr. Jakub from Głogów. Construction began in 1454 in the Gothic style. The walls of the church were built as half-timbered walls with the use of bricks, and soon after the monastery was built. According to the principle adopted by the order, the monastery complex was built outside the city walls, at the exit of one of the main routes coming out of the city. A cemetery was established next to the church (originally intended for monks but from 1643 it became public). The church (rebuilt many times 1518–1533, ca. 1620 and 1660–1667), it is a mixture of different architectural styles: the chancel is Gothic, oriented (facing east), and trihedral. The interior was Baroque in the years 1750–1753, and the late Baroque polychromes were made by the Bernardine priest Walenty Żebrowski. The façade in 1788 was acquired in the classicist style, while the bell tower from 1818 is built in the neo-Renaissance style. In 1830, the Loreto Chapel was built. It is a single-nave church with numerous side altars with a burial function. In the monastery building adjacent to the church, erected in 1514 by Jan of Komorów, in the cloister leading to the sacristy, you can see the only preserved crystal vault in Warsaw.
Additional information about Saint Anne's Church may be obtained at Wikipedia.

Details best viewed in Original Size.

St. Anne's Church is a Roman Catholic Church located in the Śródmieście district, the main center of academic chaplaincy in Warsaw. The church was built at the Bernardine monastery, which was founded by Princess Anna Fyodorówna. In 1454, through the intermediary of John of Capistrano, she brought the first monks to Warsaw. Six brothers came to Warsaw under the leadership of Fr. Jakub from Głogów. Construction began in 1454 in the Gothic style. The walls of the church were built as half-timbered walls with the use of bricks, and soon after the monastery was built. According to the principle adopted by the order, the monastery complex was built outside the city walls, at the exit of one of the main routes coming out of the city. A cemetery was established next to the church (originally intended for monks but from 1643 it became public). The church (rebuilt many times 1518–1533, ca. 1620 and 1660–1667), it is a mixture of different architectural styles: the chancel is Gothic, oriented (facing east), and trihedral. The interior was Baroque in the years 1750–1753, and the late Baroque polychromes were made by the Bernardine priest Walenty Żebrowski. The façade in 1788 was acquired in the classicist style, while the bell tower from 1818 is built in the neo-Renaissance style. In 1830, the Loreto Chapel was built. It is a single-nave church with numerous side altars with a burial function. In the monastery building adjacent to the church, erected in 1514 by Jan of Komorów, in the cloister leading to the sacristy, you can see the only preserved crystal vault in Warsaw.
Additional information about Saint Anne's Church may be obtained at Wikipedia.

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An unclassified Northwest Africa meteorite, (NWA XXX) weighing 88.5 grams.

(For scale, the black cube has sides of 1 cm).

The meteorite's shape appears somewhat oriented, so it probably maintained a fairly stable attitude during at least part of its fall through the atmosphere.

Its surface has been smoothed over time by exposure to the abrasive effects of wind-blown sand in the desert, but nevertheless, the concave face shown in this image - (probably the trailing side during stable atmospheric flight) - still retains some contraction cracks in remnant fusion crust. Contraction cracks in the fusion crust are the result of cooling during the final cold, dark part of atmospheric flight.

Four views of an unclassified Northwest Africa meteorite, (NWA XXX) weighing 88.5 grams.

(For scale, the black cube has sides of 1 cm).

The meteorite's shape appears somewhat oriented, so it probably maintained a fairly stable attitude during at least part of its fall through the atmosphere.

Its surface has been smoothed over time by exposure to the abrasive effects of wind-blown sand in the desert, but nevertheless, the concave face shown in the top left image - (probably the trailing side during stable atmospheric flight) - still retains some contraction cracks in remnant fusion crust. Contraction cracks in the fusion crust are the result of cooling during the final cold, dark part of atmospheric flight.

Gao-Guenie meteorite

Observed Fall: 5th March 1960, about 1700 hours, Burkina Faso, West Africa. (11° 39' N, 2° 11' W).

Classification: H5, ordinary chondrite.
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This specimen is a 1.8 gram flight-oriented individual - a small 'button' - with roll-over lipping. The side shown here is the trailing, or rear side with the 'roll-over lip'.

During atmospheric entry, the stone would have held a stable attitude with the leading or forward side developing a convex (curved outwards) shape as material melted and ablated away. Some of this ablated material rolled over onto the flatter, trailing side creating the roll-over lip around its rim.

[For scale, the black cube has sides of 1 cm].

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Gao-Guenie meteorites fell in a shower over the Republic of Upper Volta (now known as Burkina Faso) in West Africa at around 1700 hours on 5th March 1960. Since then, thousands of specimens have been recovered. Eyewitnesses reported that some trees were broken and henhouses destroyed.

Originally reported as two separate showers (in March and April 1960) and named separately as Gao and Guenie, the meteorites are actually indistinguishable from each other and are now considered to be from a single fall on 5th March 1960. In 1999 the names were officially fused into the collective name Gao-Guenie. [Reference the Meteoritical Bulletin No. 83].

Gao-Guenie meteorite

Observed Fall: 5th March 1960, about 1700 hours, Burkina Faso, West Africa. (11° 39' N, 2° 11' W).

Classification: H5, ordinary chondrite.
...............................

This specimen is a small, 1.8 gram, flight-oriented individual; - a small 'button' with roll-over lipping.

During atmospheric entry, the stone would have held a stable attitude with the leading or forward side developing a convex (curved outwards) shape as material melted and ablated away - (see the images at middle and lower right). The middle right image shows the leading face. The lower right picture is a side view. During hot flight through the atmosphere, some of the ablated material rolled over onto the flatter, trailing side creating a 'roll-over lip' around the rim of the trailing side - (see the image at left and top right).

[For scale, the black cube has sides of 1 cm].

................................

Gao-Guenie meteorites fell in a shower over the Republic of Upper Volta (now known as Burkina Faso) in West Africa at around 1700 hours on 5th March 1960. Since then, thousands of specimens have been recovered. Eyewitnesses reported that some trees were broken and henhouses destroyed.

Originally reported as two separate showers (in March and April 1960) and named separately as Gao and Guenie, the meteorites are actually indistinguishable from each other and are now considered to be from a single fall on 5th March 1960. In 1999 the names were officially fused into the collective name Gao-Guenie. [Reference the Meteoritical Bulletin No. 83].

Gao-Guenie meteorite

Observed Fall: 5th March 1960, about 1700 hours, Burkina Faso, West Africa. (11° 39' N, 2° 11' W).

Classification: H5, ordinary chondrite.
...............................

This specimen is a 1.8 gram flight-oriented individual - a small 'button' - with roll-over lipping. The side shown here is the trailing, or rear side with the 'roll-over lip'.

During atmospheric entry, the stone would have held a stable attitude with the leading or forward side developing a convex (curved outwards) shape as material melted and ablated away. Some of this ablated material rolled over onto the flatter, trailing side creating the roll-over lip around its rim.

[For scale, the black cube has sides of 1 cm].

................................

Gao-Guenie meteorites fell in a shower over the Republic of Upper Volta (now known as Burkina Faso) in West Africa at around 1700 hours on 5th March 1960. Since then, thousands of specimens have been recovered. Eyewitnesses reported that some trees were broken and henhouses destroyed.

Originally reported as two separate showers (in March and April 1960) and named separately as Gao and Guenie, the meteorites are actually indistinguishable from each other and are now considered to be from a single fall on 5th March 1960. In 1999 the names were officially fused into the collective name Gao-Guenie. [Reference the Meteoritical Bulletin No. 83].

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Meteorite display