Texture N°21 - Shattered and broken during the explosion

meteorite-mars.com were shattered and broken during the explosion / shockLes restes de marques d'écoulement sont visibles sur deux surfaces extérieures. Les zones non couvertes par la croûte de fusion Les restes de marques d'écoulement sont visibles sur deux surfaces extérieures. Les zones non couvertes par la croûte de fusion ont une couleur gris et une texture bloquée. Les plans de clivage sont évidents sur de grands visages en cristal et la pierre a une apparence choquée. – avec Hervé JP Chotard.

were shattered and broken during the explosion / shock vein or pocket and fusion crust

Die Nakhlite wurde nach dem Fall des Nakhla-Meteoriten bei El-Nakhla, Alexandria, Ägypten von 1911 benannt. Es handelt sich um plutonische Kumulatgesteine, die auch als Clinopyroxenite bezeichnet werden. Sie enthalten im wesentlichen Augit, ein Clinopyroxen. Es sind nur sehr wenige Nakhlite bekannt.

Meteorit Nakhla (Teilscheibe).
Achondrit, Mars-Meteorit (SNC-Gruppe), Nakhlit.

Der Meteorit besteht zu 76 - 85 % aus Augit, weiterhin sind Olivin, und akzessorisch Plagioklas, Kalifeldspat, Fe-Ti-Oxide, Pyrrhotin, Gips, Smektit, Eisenoxide, Halit, Siderit, Anhydrit und Chlorapatit vorhanden. Für die Entstehung von Nakhla und anderen Nakhliten werden verschiedene Szenarien diskutiert, sowohl eine Bildung in einer plutonischen Umgebung als auch auch an der Oberfläche in einem dicken Lavastrom oder einer oberflächennahen Intrusion. Das Gestein wurde durch Cl-haltige Fluide alteriert. Vor etwa 10.8 Millionen Jahren wurde das Material durch einen Impakt aus dem Mars herausgeschlagen.

Fall 28. Juni 1911. El Nakhla el Baharia, Nil-Delta, Ägypten. TKW 10 kg.

Größe 8,5 x 5 mm. Sammlung und Foto Thomas Witzke. http://tw.strahlen.org/fotoatlas1/meteorite_achondrite4.htmlVoir la traduction

La deuxième différence importante entre NWA 5790 et les autres nakhlites est son manque apparent de « iddingsite » (Corrigan et al. 2013 ), qui comprend des minéraux secondaires finement cristallins , y compris les carbonates, les oxydes de fer / hydroxydes, et les minéraux argileux (par exemple, Gooding et al. 1991 ; Treiman et al. 1993 ). Comme les veines contenant ces minéraux secondaires sont recoupés par croûte de fusion, ils sont clairement préterrestre, et ainsi martien d'origine (Gooding et al. 1991 ). Pour être sûr que iddingsite martien ne se produit pas dans NWA 5790, nous avons cherché à localiser, identifier et déterminer l'origine (c. -à- pré- ou post-terrestre) de tous les minéraux qui se sont formés à partir de l' eau liquide. Une conclusion que les minéraux secondaires martiens sont en effet absents de NWA 5790 suggère que la partie du corps igné dont il a été dérivé a été isolé à partir des solutions aqueuses qui interagissent avec d' autres régions du débit / seuil, et cette information peut fournir de nouvelles contraintes sur sa structure interne et l' origine.
Matériaux et méthodes

Caractérisation de l'échantillon initial

NWA 5790 comprend deux pierres (masse totale de 145 g;. Weisberg et al 2010 ), et cette étude a utilisé une seule puce de 2,7 g (~ 1,1 x 1,2 x 0,8 cm 3 ) de la partie extérieure de l' une des pierres qui ont été acquises à partir de la collection Macovich. Cet échantillon a été sélectionné car il fournit un profil de l'extérieur de la météorite (qui est le plus susceptible de contenir des produits d'altération terrestres) à l'intérieur frais. Surface extérieure d' origine de la météorite a un revêtement de couleur chamois à grains fins qui Shih et al. ( 2010 ) appelé « caliche » (Fig. 1 a), tandis que les surfaces intérieures fraîchement cassés de la puce sont de couleur vert foncé (Fig. 1 b). Comme l'intérieur de la météorite est libre de Fe- (hydr) veines d'oxyde et des jantes de grains, il serait classé comme W0 sur la section mince échelles aux intempéries (Jull et al. 1991 ; Wlotzka 1993 ;. Al-Kathiri et al 2005 ) . Étant donné que les minéraux d'une origine terrestre présumée sont visibles à l'œil nu sur la surface extérieure de l' échantillon ( à savoir le « caliche »), NWA 5790 devrait avoir une sous - classification « E ».

http://onlinelibrary.wiley.com/doi/10.1111/maps.12424/full

http://www.nhm-wien.ac.at/.../hall_1.../minerals_meteorites
chassigny
Martian meteorite which fell on 3 October 1815 in France. The Chassigny meteorite is the first Martian meteorite that has entered meteorite collections, in 1815-1820s, even though its Martian origin was only recognized in the 1980s. The displayed piece is the second largest known worldwide.
gnetitehould never attempt to visit any sites listed in mindat.org without first ensuring that you have the permission of the land and/or mineral rights holders for access and that you are aware of all safety precautions necessary.
References

Mason, B., Nelson, J. A., Muir, P., & Taylor, S. R. (1976). The composition of the Chassigny meteorite. Meteoritics 11(1): 21-27.

Floran, R. J., Prinz, M., Hlava, P. F., Keil, K., Nehru, C. E., & Hinthorne, J. R. (1978). The Chassigny meteorite: A cumulate dunite with hydrous amphibole-bearing melt inclusions. Geochimica et Cosmochimica Acta, 42(8), 1213-1229.

McSween, H.Y.,Jr. (1987) Meteorites and their Parent Planets. Cambridge University Press: Cambridge, New York, Melbourne 237 pp.

McSween, H.Y.,Jr (1994). What we have learned about Mars from the SNC Meteorites: Meteoritics 29(6): 757-779. (Nov 1994)

Wentworth, S. J., & Gooding, J. L. (1994). Carbonates and sulfates in the Chassigny meteorite: Further evidence for aqueous chemistry on the SNC parent planet. Meteoritics 29(6): 860-863. (Nov 1994)

Langenhorst, F. & Greshake, A. (Jan 1999) A transmission electron microscope study of Chassigny: Meteoritics & Planetary Science 34 (1):43-59. (Jan 1999).

Grady, M. M. (2000). Catalogue of Meteorites (5/e). Cambridge University Press: Cambridge, New York, Oakleigh, Madrid, Cape Town. 690 pages.

McSween, H. Y. Jr. (2002) The rocks of Mars, from far and near. Meteoritics & Planetary Science 37 (1): 7–25. (Jan 2002)

McCubbin, F. M., & Nekvasil, H. (2008). Maskelynite-hosted apatite in the Chassigny meteorite: Insights into late-stage magmatic volatile evolution in martian magmas. American Mineralogist, 93(4), 676-684.

External Links

http://www.geocities.com/~dweir/
http://www.lpi.usra.edu/meteor/metbull.php
http:www.lpi.usra.edu/meteor/metbull.php?code=5331 - Chassigny@MetBullDatabase

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Comparatifs textures Martian Météorite examples Météorite CH NAK Chizé and Chassignite NWA 8694 (a single 54.80g)
Chassignite NWA 8694, martian meteorite, Mars Meteorite 0.162g part slice
Weight : 0.162 g Size : 7 x 4 mm

1 180,00 USD
Environ 1 103,27 EUR
http://www.ebay.fr/itm/Chassignite-NWA-8694-martian-meteorite-Mars-Meteorite-0-162g-part-slice-/321811749106

The missing link between the Chassignites and Nakhlites?

This is a cumulate dunite (85% olivine) with an adcumulate texture with small patches rich in interstitial material having an orthocumulate texture

Part slice with fusion crust

Weight : 0.162 g Size : 7 x 4 mm

Accompanied by a display box and certificate of authenticity
I am the owner of the NWA 8694 chassignite, follow me on FaceBook > Labenne Meteorites on FaceBook

NORTHWEST AFRICA 8694, A FERROAN CHASSIGNITE. R.H. Hewins1,2, B. Zanda1,2, S. Pont1, M. Hu- mayun.3, N. Assayag3 and P. Cartigny3. 1IMPMC, MNHN, 75005 Paris, FR. 2Rutgers University, Piscataway, NJ
08854, USA. 3Florida State University, Tallahassee, FL 32310, USA. 4IPGP, Univ. Paris Diderot, F-75005 Paris, FR.

http://www.hou.usra.edu/meetings/lpsc2015/pdf/2249.pdf

From the Meteoritical Bulletin > http://www.lpi.usra.edu/meteor/metbull.php?code=61276

Northwest Africa 8694 (NWA 8694)
Morocco
Purchased: 14 July 2014
Classification: Martian meteorite (Chassignite)
Physical characteristics: A single 54.80g flattened spherical stone, almost entirely covered by fusions crust.
Petrography: (R. Hewins, S. Pont, B. Zanda, MNHNP) This meteorite is a cumulate dunite with 85% highly fractured olivine. It has an adcumulate texture with small patches rich in interstitial material having an orthocumulate texture. The main intercumulus phases are pigeonite and augite, both with very fine (1 μm) exsolution lamellae,and glass. Minor phases include chromite, partly enclosed by olivine, and ilmenite. The olivine contains largely crystalline melt inclusions, surrounded by radial fractures. The main phases in melt inclusions are orthopyroxene and glass; rare phases include apatite, amphibole and mica.
Geochemistry: Mineral compositions: (R. Hewins, MNHNP) The olivine composition is Fo53.2±0.3Fa46.8±0.3, with an FeO/MnO ratio of 50.0±1.6, n=24. The crystals are equilibrated in Fe-Mg, but retain a weak depletion of Ca towards crystal rims, with a total range of 0.8–0.29 wt. % CaO. The pigeonite composition is En55.8±0.9Fs37.5±1.0Wo6.7±1.3, n=26, and FeO/MnO of 28.7±1.9; the orthopyroxene is En59.9±0.4Fs37.7±0.9Wo2.4±0.8 and FeO/MnO ratio of 30.2±3.0; and the augite is En40.6±0.2Fs16.1±0.6Wo43.3±0.5, with an FeO/MnO ratio of 27.4±3.2, (neglecting overlap compositions). The orthopyroxene in the melt inclusions varies from En56 to En59, with Al2O3 up to 4 wt.%, whereas interstitial orthopyroxene has only 0.4±0.3 wt.% Al2O3. The amphibole is calcium-rich with 3% TiO2 and the mica is phlogopitic. Apatite has about 2.5 wt.% of each of F and Cl. Geochemistry: (N. Asseyag, P. Cartigny, IPGP). Oxygen isotope analysis gives δ18O=4.74 δ17O=2.78 Δ17O=0.32, (standard errors: ±0.10, ±0.07, ±0.04 respectively).
Classification: (R. Hewins, S. Pont and B. Zanda, MNHNP) The meteorite is classified as a chassignite. The textures and mineral assemblages are almost identical to those of Chassigny and NWA 2737. The olivine and pyroxene compositions are intermediate between those of Chassigny and Nakhla. The Fe/Mn ratios of olivine grains fall on to just above the Papike reference line for Mars. Specimens: Specimen: 12.3 g at MNHNP
Chassignite / Mars Meteorite
Synonyms: olivine achondrites, martian dunites

General: This group is named for Chassigny, a meteorite that fell in France in 1815. In the early days of meteoritics nobody suspected that it would become one of the key samples in the future, and thus most of it was subsequently lost. Only a bit more than 600 grams of the original 4 kilos of Chassigny have been preserved up to this day, and until more recently, when a second chassignite, NWA 2737, was recovered from the deserts of Africa, only small crumbs of this ultra-rare class of martian meteorites were available to institutions, museums, and private collectors.
Description: The chassignites are medium- to fine-grained ultra-mafic rocks, resembling terrestrial dunites and peridotites. The color of their interiors varies: the original Chassigny is a light-green rock with only minor black spots in its matrix while NWA 2737 has a more dark appearance, with blueish glas veins quenched in a shock-blackened matrix. The fusion crust on Chassigny is black while NWA 2737 doesn't show remnant fusion crust due to terrestrial weathering.
Mineralogy: Chassignites are cumulate rocks, resembling terrestrial dunites, and peridotites. They consist of about 90% Fe-rich olivine, minor clinopyroxene, plagioclase, chromite, melt inclusions, and other accessory minerals and phases. Melt inclusions in Chassigny contain rare amphiboles, and cracks within the rock are often filled with carbonate and sulfate salts, indicating a mild pre-terrestrial aqueous alteration. The new chassignite, NWA 2737 has just been officially classified, and thus we don't have too much data on it, so far. It resembles the original Chassigny in many aspects, but it also differs in others, e.g., in its shock level. NWA 2737 displays shock-blackened olivines that haven't been witnessed in any terrestrial or extra-terresrial rock type, thus far.
Formation history: Crystallization ages of about 1.36 billion years, and compositional and elemental trends indicate a relationship between the chassignites and the nakhlites, suggesting an origin from the same parent magma on Mars. However, the chassignites show noble gas values different from those found in other SNC members or in the martian atmosphere. It is suspected that these gases might originate from the martian mantle, suggesting a formation within magma plutons deep inside the martian crust for the chassignites.
Origin: Planetary. Comparisons between various characteristics of the members of the SNC group, and data obtained about Mars by space probes and landers, such as Viking, Pathfinder, and the new Mars rovers Spirit and Opportinity, have provided strong proof for the martian origin of the SNCs, and today it is widely accepted that these achondrites actually represent genuine Mars rocks that have been blasted off of the surface of the Red Planet by major impacts. Recent studies, based on data provided by the Mars Odyssey Orbiter, and THEMIS (Thermal Emission Imaging System), suggest that both, the nakhlites, and the chassignites, were ejected from a large impact crater in the northeast region of the Syrtis Major volcanoes.
Members: For nearly 200 years Chassigny remained the only representative of its own class, in 2000 a second chassignite has been recovered from Northwest Africa the NWA 2737 (611g in nine pieces lacking fusion crust). More recently in 2014 a third chassignite has been recovered, the NWA 8694 a single 54.8g stone covered by fusion crust. copyright@Luc Labenne

BSE of the NWA 8694 chassignite copyright Sylvain Pont

0.jpg

Labenne Meteorites is a private organization specialized in finding and supplying meteorites to institutions and private collectors.

Every year since the 1970s, governments have sponsored expeditions to retrieve meteorites in Antarctica. However, it has only been since the 1990s that warm deserts like the Sahara have revealed their remarkable discovery potential. Our numerous finds are certainly witness to this fact. Through systematic and dedicated searching, we have found thousands of meteorites – many of which have attracted serious scientific interest.

In addition to the Lunar and Martian specimens from various space exploration missions, Lunar and Martian meteorites arrive on Earth from unexplored, uncharted regions of the Moon and Mars, and inspire extensive research.

Interest in such exceptional meteorites is on the rise in both the scientific community and the general public, as fascination for all things related to Space, particularly Mars and the Moon, goes sky-high.

Our Scientific Roots

Over the last eight years, we’ve organized expeditions to find and collect new meteorites in the warm deserts of the world, primarily the Sahara and Oman. Our expeditions have led us to discover several thousand new meteorites, known by the names Sahara and Dhofar. They have been the object of extensive scientific research in the world’s largest universities, research institutes and museums in Europe, the United States and Japan. Our finds are exhibited in the most prestigious collections in the world – the Natural History Museum in London, the Museum National d'Histoire Naturelle in Paris, Das Naturhistorische Museum Wien in Vienna, Museum Für Naturkunde in Berlin, American Museum of National History in New York, Chicago Field Museum in Chicago.

We are members of the Meteoritical Society, the official organization governing the classification and reference of new meteorites affiliated with the Department of Chemistry and Biochemistry of the University of Arkansas, in the United States. The Meteoritical Society is also responsible for the scientific journal Meteoritics and Planetary Science, entirely devoted to meteorite research.

Luc Labenne

More meteorites for sale, visit http://www.meteorites.tv/ ,"Meteorites For Science, Education & Collectors" ~ 700 Meteorites For Sale » Search in The Meteorite Classification Index Table

– avec Hervé JP Chotard.

A slice of a Martian meteorite, which was discovered in Dar al Gani, Sahara Desert, Libya, on May 1, 1998. Its spinach-green matrix is interspersed through with black olivine phenocrysts. THANK S

Photo: Heritage Auctions

http://gizmodo.com/30-starry-wonders-hiding-inside-of...

meteorite-mars.com
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Pas dans le journal
Chassignite NWA 8694 (a single 54.80g)
Chassignite NWA 8694, martian meteorite, Mars Meteorite 0.162g part slice
Weight : 0.162 g Size : 7 x 4 mm

1 180,00 USD
Environ 1 103,27 EUR
http://www.ebay.fr/.../Chassignite-NWA-8694.../321811749106

The missing link between the Chassignites and Nakhlites?

This is a cumulate dunite (85% olivine) with an adcumulate texture with small patches rich in interstitial material having an orthocumulate texture

Part slice with fusion crust

Weight : 0.162 g Size : 7 x 4 mm

http://www.meteoritestudies.com/protected_CHASSIG.HTM There are only four Calcium poor Martian Meteorites in the world - ALH84001, Chassigny, Dhofar 378, and NWA 998

The Chassigny meteorite is the first Martian meteorite that has entered meteorite collections, in 1815-1820s, even though its Martian origin was only recognized in the 1980s. The displayed piece is the second largest known worldwide.
gnetitehould never attempt to visit any sites listed in mindat.org without first ensuring that you have the permission of the land and/or mineral rights holders for access and that you are aware of all safety precautions necessary.
References

Mason, B., Nelson, J. A., Muir, P., & Taylor, S. R. (1976). The composition of the Chassigny meteorite. Meteoritics 11(1): 21-27.

textures Martian Météorite CH Chizé the différentes textures Chassignites Naklites Météorites – avec Hervé JP Chotard.

Chassignite
(dunite)
La météorite de Chassigny représente le spécimen type du groupe des Chassignites. Elle a longtemps constitué le seul exemplaire de ce groupe jusqu'à la découverte de NWA 2737. Sa chute a été observée en France en 1815 près du village de Chassigny sur le plateau de Langres (Haute-Marne), à une époque ou la véritable nature des météorites venait seulement d'être comprise (la chute historique de la météorite de l'Aigle remonte au 26 avril 1803). La Chassignite est tombée le même jour que celle de Zagami, un 3 octobre. Si elle pesait à l'origine 4 kilos, la majeure partie a été perdue, et nous ne disposons plus à l'heure actuelle que de 570 grammes de roche martienne.
https://www.nirgal.net/snc/chassigny.html
Notre Chassignite est un cumulat, c'est à dire une roche formée par l'accumulation dense d'un ou plusieurs minéraux au fond d'une chambre magmatique. Ici, la roche est presque exclusivement composée d'olivine, ce qui en fait une dunite. Sa composition est la suivante : 91,6 % d'olivine riche en fer, 5 % de pyroxène, 1,7 % de plagioclase et 1,4 % de chromite (riche en Fe3+). Elle renferme également 0,3 % d'inclusions vitreuses (observables par exemple dans les cristaux d'olivine), dans lesquelles on distingue parfois des amphiboles riches en titane (kaersutite). On trouve enfin une foule de minéraux accessoires en très petites quantités : feldspaths alcalins, biotite, oxydes (ilménite, rutile, baddeleyite), sulfures (marcasite, pentlandite, troilite) et phosphates (chlorapatite). Les fractures qui parcourent la roche sont obstruées par des carbonates et des sulfates, ce qui atteste d'une altération par de l'eau liquide.

Chassigny, Stein, SNC / Chassignit
Fall 3.Oktober 1815 Haute Mame, France
Gesamt ca. 4 kg
<1 mg = (49, -) http://www.jgr-apolda.eu/.../METS/METMOMA/METAL_MS.HTM

Bildbreite

Météorite Chizé de Mars Communauté http://www.meteoritestudies.com/protected_CHASSIG.HTM There are only four Calcium poor Martian Meteorites in the world - ALH84001, Chassigny, Dhofar 378, and NWA 99